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"ecliptic" Definitions
  1. of or relating to the ecliptic or an eclipse
  2. the great circle of the celestial sphere that is the apparent path of the sun among the stars or of the earth as seen from the sun : the plane of the earth's orbit extended to meet the celestial sphere
"ecliptic" Synonyms
gyre aureole band belt bowl bracelet circlet circuit circumference circus cirque coil compass cordon corona crown cycle disc(UK) disk(US) enclosure

1000 Sentences With "ecliptic"

How to use ecliptic in a sentence? Find typical usage patterns (collocations)/phrases/context for "ecliptic" and check conjugation/comparative form for "ecliptic". Mastering all the usages of "ecliptic" from sentence examples published by news publications.

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If the moon crosses the ecliptic when full, we&aposll get an eclipse of the moon; if the moon crosses the ecliptic when new, we&aposll get an eclipse of the sun.
Moreover, these perihelia all lie near the ecliptic—the plane of Earth's orbit and also, approximately, that of the other planets—while the objects' orbits are all angled at 30° below the ecliptic.
Its orbit doesn't lie in the plane of the ecliptic.
There's an imaginary line that circles the sky called the ecliptic.
The ecliptic passes through 13 of the 88 constellations in the sky.
This Saturday's half moon in Libra marks the halfway point between the two ecliptic events.
Eclipses only occur at times when the Moon is full or new when it crosses the ecliptic.
Your sign denotes where along the ecliptic the sun was at your birth, relative to these segments.
Eventually, if funding permits, the K2 mission will observe every part of the cosmos along the ecliptic.
Like the Earth, Jupiter's orbit around the Sun lies in a particular plane (the "Plane of the Ecliptic").
And the dot is redder if the Moon is closer to the Plane of the Ecliptic that day.
Incidentally, this is the reason the sun&aposs path around the sky is called the "ecliptic" — for "eclipse"!
The planets and the moon follow roughly the same path through the sky, which is called the ecliptic.
Their locations along the ecliptic can change like beads on a hoop, whereas the stars appear to remain fixed.
But depending on the angle of its orbit, it might also leave the ecliptic and avoid death by smashing.
Indeed, after swinging around the Sun, it passed about 25m km below Earth, before speeding back above the ecliptic plane.
A flyby of Venus in 21859 will swing Solar Orbiter out of the ecliptic to an angle of 22 degrees.
Image: NASA With the K22 mission, we can now look at points all along the ecliptic (plane of the Solar System).
The ecliptic is the plane of the solar system on which all the planets orbit the sun, and the moon travels nearby.
She sent along a book manuscript, titled "The Darkening Ecliptic," containing all the poems that Stewart and McAuley had written for the occasion.
It flew in south of the ecliptic, shedding cold mass in irregular bursts like a black comet—a deceleration maneuver that took three years.
In celebration of the name change, the Planetary Society released a new video showing a sail deployment test at Ecliptic Enterprises Corporation in Pasadena.
Instead of staring at one field for four years, the telescope is staring at different points along the ecliptic for about 80 days each.
It dove out of deep space almost perpendicular to the plane of the ecliptic — the plane around the sun's equator where all the planets orbited.
Until now, almost all of the solar-watching spacecraft have orbited in the ecliptic, or the same plane that the planets travel around the sun.
On March 9th, a new Moon will sweep across the Pacific in the ecliptic plane; that is, the plane in which the Earth orbits the Sun.
Solar eclipses only happen when a new Moon occurs on a day when its orbit intersects the ecliptic, the path the Sun traces across the sky.
After swinging around the Sun, as the diagram shows, it passed about 25m km below Earth on October 14th, before speeding back above the ecliptic plane.
Additional flybys — one of Earth, two more of Venus — will further adjust the orbit, which will still be in the ecliptic, the plane of the orbits.
Earth is at the center of the coin; the nodes are the two points on the coin&aposs rim that are on the same ecliptic plane as Earth.
The DES is particularly good at finding "high-inclination" objects, which means TNOs that orbit at a relatively sharp angle to the ecliptic plane of the solar system.
The basic point is that there's a solar eclipse whenever the Moon is both positioned between the Earth and the Sun, and it's in the Plane of the Ecliptic.
However, the latter's trajectory caused it to exit the ecliptic (the flat disk in which most of the solar system's objects are found) earlier and at a different angle.
I think Coma Ecliptic is us figuring out how to sound, figuring out how to make the music we want to make and making it work pretty much flawlessly.
One of the fragmentary Babylonian texts (left) showing a portion of a calculaton for determining Jupiter's displacement across the ecliptic plane as the area under a time-velocity curve (right).
What's more, all of their orbits are all tilted the same direction, pointing about 30 degrees down relative to the ecliptic plane (the plane in which planets orbit the Sun).
Here's the Moon going around the Earth, colored red whenever it's close to the Plane of the Ecliptic: Now let's look at what happens over the course of about a year.
By now, with the moon a quarter of a million miles from Earth, the sun's gravity should have tipped the moon's orbit to lie in the same plane as the ecliptic.
Like I feel The Silent Circus was a little inauthentic, but looking at the whole journey, I feel like everything has been this natural evolution, natural steps forward, culminating with Coma Ecliptic.
The hypothesis, published by a pair of Caltech researchers, says the planet is probably a gas giant that was punted out of the ecliptic plane, in which all the other planets orbit, eons ago.
Since the spring of 2014, Kepler has moved across the plane of our solar system (the ecliptic plane), observing different parts of the northern and southern hemisphere skies for 80 days at a time.
The display is made possible by the uncommon alignment of all five planets along what is called the "ecliptic" plane of their orbits, according to Jim Green, the planetary science division director at NASA.
Via Mathieu OssendrijverThe now-decoded "text A" describes a procedure for calculating Jupiter's displacement across the ecliptic plane, the path that the Sun appears to trace through the stars, over the course of a year.
After about six months, the team made a case to NASA for a mission that would stare across the ecliptic plane (the plane in which planets orbit the Sun), observing different regions of the sky.
Nor could its velocity have been the result of the extra gravitational kick provided by an encounter with a planet, since it arrived from well above the ecliptic plane near which all the Sun's planets orbit.
They don't happen every time there's a full moon because the Moon's orbit is tilted relative to the ecliptic plane, the path the Earth travels around the Sun or the path the Sun travels through the sky.
Nor could its velocity have been the result of an encounter with a planet giving it an extra gravitational kick, for it arrived from well above the ecliptic plane, close to which all the Sun's planets orbit.
Most of the members of Delaware's Scorched weren't even in elementary school when old school death metal was known as just plain "death metal," but their 2018 album Ecliptic Butchery recaptures the sound and fury of old perfectly.
In fact, the moon will reach the descending node of its orbit — the point where it crosses the ecliptic going from north to south — just 21975 minutes after it arrives at full phase, resulting in a nearly central total eclipse.
At that moment, the sun's position in the sky is exactly where the ecliptic (the path the planets take as they move through the constellations) crosses the celestial equator (the projection of the Earth's own equator onto the celestial sphere).
They also noticed that the Moon went above and below the Plane of the Ecliptic (now known to be because of the inclination of its orbit)—with an average period (the so-called draconic month) that they measured as about 27.21 days.
For the telescope's next act, the satellite is expected to take a look at some areas already seen and observe the ecliptic, the part of the sky covered by the Sun's path throughout the year, TESS scientist Sara Seager told Axios via email.
At that moment, the sun's position in the sky is exactly where the ecliptic (the plane of the solar system and the path that the planets take as they move through the constellations) crosses the celestial equator (the projection of the Earth's own equator onto the celestial sphere).
In advance of Rogue One: A Star Wars Story, a new book—Death Star Owner's Technical Manual—lays bare the plans for the station that, presumably, get stolen by rebels, transmitted to Princess Leia, secreted in an R2 unit on board the Rand Ecliptic, and eventually made possible the Death Star's destruction.
The moon&aposs orbit is tilted toward Earth&aposs at an angle of just over 5 degrees, and the nodes are the two points at which the planes intersect — that is, at which the moon passes down or up through the plane that Earth revolves around the sun on, called the  ecliptic plane .
In their commercials, Google, Amazon, and Apple's marketers have chosen to sell the public on the usefulness of voice assistants not by enacting the verbal exchanges that we might have with our devices, but by drawing our attention either to the absence of them — what life is like without the Google Assistant or the "real" Alexa — or to the ecliptic power of another mode of expression — music, as curated by Siri.
Earth-centered ecliptic coordinates as seen from outside the celestial sphere. Ecliptic longitude (red) is measured along the ecliptic from the vernal equinox. Ecliptic latitude (yellow) is measured perpendicular to the ecliptic. A full globe is shown here, although high-latitude coordinates are seldom seen except for certain comets and asteroids.
The ecliptic coordinate system specifies positions relative to the ecliptic (Earth's orbit), using ecliptic longitude and latitude. Besides the equatorial and ecliptic systems, some other celestial coordinate systems, like the galactic coordinate system, are more appropriate for particular purposes.
The ecliptic is an important reference plane and is the basis of the ecliptic coordinate system.
This is the actual intersection of the two planes at any particular moment, with all motions accounted for. A position in the ecliptic coordinate system is thus typically specified true equinox and ecliptic of date, mean equinox and ecliptic of J2000.0, or similar. Note that there is no "mean ecliptic", as the ecliptic is not subject to small periodic oscillations.
The fundamental plane is the plane of the Earth's orbit, called the ecliptic plane. There are two principal variants of the ecliptic coordinate system: geocentric ecliptic coordinates centered on the Earth and heliocentric ecliptic coordinates centered on the center of mass of the Solar System. The geocentric ecliptic system was the principal coordinate system for ancient astronomy and is still useful for computing the apparent motions of the Sun, Moon, and planets.Aaboe, Asger.
Due to a 41° orbital inclination, it is above the ecliptic plane when crossing Jupiter's orbit, and below the ecliptic when crossing Saturn's orbit.
Heliocentric ecliptic coordinates. The origin is the Sun's center, the plane of reference is the ecliptic plane, and the primary direction (the -axis) is the vernal equinox. A right-handed rule specifies a -axis 90° to the west on the fundamental plane. The -axis points toward the north ecliptic pole.
Right ascension for "fixed stars" near the ecliptic and equator increases by about 3.05 seconds per year on average, or 5.1 minutes per century, but for fixed stars further from the ecliptic the rate of change can be anything from negative infinity to positive infinity. The right ascension of Polaris is increasing quickly. The North Ecliptic Pole in Draco and the South Ecliptic Pole in Dorado are always at right ascension 18h and 6h respectively.
The annual path that the Sun appears to follow against the background of relatively fixed stars is known as the ecliptic. Since the Moon's orbit is inclined 5.14° to the ecliptic, the Moon will always remain within about 5° north or south of the ecliptic. For half of a sidereal month (with respect to the stars), the Moon is either north or south of the ecliptic. The two points where the Moon's orbit intersects that of Earth are called the lunar nodes; at the ascending node, the Moon moves north of the ecliptic, while at the descending node, the satellite moves south.
Astronomical latitude is not to be confused with declination, the coordinate astronomers use in a similar way to specify the angular position of stars north/south of the celestial equator (see equatorial coordinates), nor with ecliptic latitude, the coordinate that astronomers use to specify the angular position of stars north/south of the ecliptic (see ecliptic coordinates).
The apparent motion of the Sun along the ecliptic (red) as seen on the inside of the celestial sphere. Ecliptic coordinates appear in (red). The celestial equator (blue) and the equatorial coordinates (blue), being inclined to the ecliptic, appear to wobble as the Sun advances. The celestial equator and the ecliptic are slowly moving due to perturbing forces on the Earth, therefore the orientation of the primary direction, their intersection at the Northern Hemisphere vernal equinox, is not quite fixed.
At such conjunction both objects have the same ecliptic longitude. Conjunction in right ascension and conjunction in ecliptic longitude do not normally take place at the same time, but in most cases nearly at the same time. However, at triple conjunctions, it is possible that a conjunction only in right ascension (or ecliptic length) occurs. At the time of conjunction – it does not matter if in right ascension or in ecliptic longitude – the involved planets are close together upon the celestial sphere.
One definition of the tropical year would be the time required for the Sun, beginning at a chosen ecliptic longitude, to make one complete cycle of the seasons and return to the same ecliptic longitude.
The Moon's rotational axis precesses so as to trace out a cone that intersects the ecliptic plane as a circle. # A plane formed from a normal to the ecliptic plane and a normal to the Moon's orbital plane will contain the Moon's rotational axis. In the case of the Moon, its rotational axis always points some 1.5 degrees away from the North ecliptic pole. The normal to the Moon's orbital plane and its rotational vector are always on opposite sides of the ecliptic plane.
Earth's axial tilt (obliquity) is currently about 23.4°. Earth's orbital plane is known as the ecliptic plane, and Earth's tilt is known to astronomers as the obliquity of the ecliptic, being the angle between the ecliptic and the celestial equator on the celestial sphere. It is denoted by the Greek letter ε. Earth currently has an axial tilt of about 23.44°.
Eclipses occur at these points, hence the name ecliptic. The nodes precess around the ecliptic axis at the rate of one circuit every 18.6 years. The ecliptic makes the steepest angle to the horizon at the equinoxes. Since the crescent Moon appears near the Sun, the crescent would appear to lie on its back when low above the horizon around the equinoxes.
At this time Ulysses had a low orbital inclination to the ecliptic.
On March 17, 2015 they announced that Coma Ecliptic will be released through Metal Blade Records on July 7, 2015, and released a song titled "Memory Palace". It was later released July 10, 2015. From 2015 - 2017, Between the Buried and Me went out on their Coma Ecliptic World Tour and headlined with / co-headlined for August Burns Red, Animals as Leaders, Devin Townsend Project, Fallujah, Enslaved and The Contortionist. The band released "Coma Ecliptic: Live" on April 28, 2017, which has their entire "Coma Ecliptic" album played live in its entirety.
In 2007, she premiered a long poem "Ecliptic", with flute, harp and birdsong.
360px :NGC 2392 is located just east of δ Geminorum, just south the ecliptic.
Star map with the Pleiades (upper right) and the Hyades (centre, V-shaped head of the constellation Taurus with its main star Aldebaran, γ Tauri und ε Tauri (Ain)) at both sides of the ecliptic line (dashed red). The Golden Gate of the Ecliptic is an asterism in the constellation Taurus that is known for several thousand years. The constellation is built by the two eye-catching open star clusters of the Pleiades and the Hyades that form the two post of a virtual gate at the two sides of the ecliptic line. Since all planets as well as the moon and the sun always move very closely along the virtual circle of the ecliptic, all these seven orbiting bodies are regularly passing through the Golden Gate of the Ecliptic.
Stars at the ecliptic poles appear to move in circles, stars exactly in the ecliptic plane move in lines, and stars at intermediate angles move in ellipses. Shown here are the apparent motions of stars with the ecliptic latitudes corresponding to these cases, and with ecliptic longitude of 270°. The direction of aberration of a star at the northern ecliptic pole differs at different times of the year Annual aberration is caused by the motion of an observer on Earth as the planet revolves around the Sun. Due to orbital eccentricity, the orbital velocity v of Earth (in the Sun's rest frame) varies periodically during the year as the planet traverses its elliptic orbit and consequently the aberration also varies periodically, typically causing stars to appear to move in small ellipses.
IERS EOP PC Useful constants. Today the mean tropical year is defined as the period of time for the mean ecliptic longitude of the Sun to increase by 360 degrees.Richards, E.G. (2013). Calendars. In S.E. Urban & P.K. Seidelmann (Eds.), Explanatory Supplement to the Astronomical Almanac (3rd ed.). Mill Valley, CA: University Science Books. p. 586. Since the Sun's ecliptic longitude is measured with respect to the equinox,"longitude, ecliptic" and "dynamical equinox". (2018).
' has a highly inclined orbit typical of scattered objects and orbits nearly perpendicular to the ecliptic.
The nodical period is the period between two crossings of the ecliptic in the same direction.
Its orbit has an eccentricity of 0.13 and an inclination of 6° with respect to the ecliptic.
The modelling also gave two poles at (343.0°, −74.0°) and (133.0°, −75.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.08 and an inclination of 3° with respect to the ecliptic.
Its orbit has an eccentricity of 0.06 and an inclination of 20° with respect to the ecliptic.
Its orbit has an eccentricity of 0.03 and an inclination of 7° with respect to the ecliptic.
Its orbit has an eccentricity of 0.03 and an inclination of 17° with respect to the ecliptic.
Its orbit has an eccentricity of 0.06 and an inclination of 4° with respect to the ecliptic.
Its orbit has an eccentricity of 0.09 and an inclination of 5° with respect to the ecliptic.
Its orbit has an eccentricity of 0.03 and an inclination of 6° with respect to the ecliptic.
Its orbit has an eccentricity of 0.07 and an inclination of 11° with respect to the ecliptic.
Its orbit has an eccentricity of 0.11 and an inclination of 9° with respect to the ecliptic.
Two spin axes at (62.0°, −66.0°) and (231.0°, −74.0°) in ecliptic coordinates (λ, β) were also determined.
Its orbit has an eccentricity of 0.13 and an inclination of 8° with respect to the ecliptic.
Its orbit has an eccentricity of 0.14 and an inclination of 1° with respect to the ecliptic.
Its orbit has an eccentricity of 0.02 and an inclination of 1° with respect to the ecliptic.
Its orbit has an eccentricity of 0.03 and an inclination of 6° with respect to the ecliptic.
Its orbit has an eccentricity of 0.11 and an inclination of 16° with respect to the ecliptic.
In the Sky Earth astronomy reference utility showing the ecliptic and relevant date as at J2000 - present.
Its orbit has an eccentricity of 0.03 and an inclination of 8° with respect to the ecliptic.
Obliquity of the ecliptic is the term used by astronomers for the inclination of Earth's equator with respect to the ecliptic, or of Earth's rotation axis to a perpendicular to the ecliptic. It is about 23.4° and is currently decreasing 0.013 degrees (47 arcseconds) per hundred years because of planetary perturbations. , art. 365–367, p. 694–695, at Google books The angular value of the obliquity is found by observation of the motions of Earth and other planets over many years.
The study also determined two spin axes of (96.0°, 30.0°) and (283.0°, 35.0°) in ecliptic coordinates (λ, β).
The study also determined two spin axes of (201.0°, −41.0°) and (2.0°, −36.0°) in ecliptic coordinates (λ, β).
The study also determined two spin axes of (249.0°, −52.0°) and (51.0°, −61.0°) in ecliptic coordinates (λ, β).
The team also determined two spin axis of (248.0°, 56.0°) and (54.0°, 48.0°) in ecliptic coordinates (λ, β) ().
The study also determined two spin axis of (231.0°, −56.0°) and (71.0°, −60.0°) in ecliptic coordinates (λ, β).
One study also found two spin axis of (72.0°, −84.0°) and (265.0°, −46.0°) in ecliptic coordinates (λ, β).
The study also determined two spin axes of (145.0°, −63.0°) and (320.0°, −70.0°) in ecliptic coordinates (λ, β).
The study also determined two spin axes of (202.0°, −66.0°) and (64.0°, −27.0°) in ecliptic coordinates (λ, β).
Since it is near the ecliptic, it can be occulted by the Moon and very rarely by planets.
A star that is precisely at one of the ecliptic poles (at 90° from the ecliptic plane) will appear to move in a circle of radius \kappa about its true position, and stars at intermediate ecliptic latitudes will appear to move along a small ellipse. For illustration, consider a star at the northern ecliptic pole viewed by an observer at a point on the Arctic Circle. Such an observer will see the star transit at the zenith, once every day (strictly speaking sidereal day). At the time of the March equinox, Earth's orbit carries the observer in a southwards direction, and the star's apparent declination is therefore displaced to the south by an angle of \kappa.
The studies also determined a spin axis at (296.0°, 41.0°) and (294.0°, 41.0°) in ecliptic coordinates (λ, β), respectively.
Its orbit has a notably high eccentricity of 0.19 and an inclination of 14° with respect to the ecliptic.
The angle between the Earth's equatorial plane and the ecliptic, ε, is called the obliquity of the ecliptic and ε ≈ 23.4°. An equinox occurs when the earth is at a position in its orbit such that a vector from the earth toward the sun points to where the ecliptic intersects the celestial equator. The equinox which occurs near the first day of spring (with respect to the North hemisphere) is called the vernal equinox. The vernal equinox can be used as a principal direction for ECI frames.
It gave a concurring sidereal period of hours and a spin axis at (355.0°, −78.0°) in ecliptic coordinates (λ, β).
Explorer 34 was placed into a high-inclination, highly eccentric earth orbit. The apogee point was located near the ecliptic plane and had an initial local time of about 1,900 hours. The spacecraft was spin-stabilized and had an initial spin period of 2.6 seconds. The spin vector was approximately perpendicular to the ecliptic plane.
Ariadne is very elongate (almost twice as long as its smallest dimension) and probably bi-lobed or at least very angular. It is a retrograde rotator, although its pole points almost parallel to the ecliptic towards ecliptic coordinates (β, λ) = (−15°, 253°) with a 10° uncertainty. This gives an axial tilt of about 105°.
The correction is small for objects at the poles of the ecliptic. Elsewhere, it is approximately an annual sine curve, and the highest amplitude occurs on the ecliptic. The maximum correction corresponds to the time in which light travels the distance from the barycentre to the Earth, i.e. ±8.3 min (500 s, 0.0058 days).
To find the date, find the place where the hour hand or sun disk intersects the ecliptic dial: this indicates the current star sign, the sun's current location on the ecliptic. The intersection point slowly moves around the ecliptic dial during the year, as the sun moves out of one astrological sign into another. In the diagram showing the clock face on the right, the sun's disk has recently moved into Aries (the stylized ram's horns), having left Pisces. The date is therefore late March or early April.
A slow motion of Earth's axis, precession, causes a slow, continuous turning of the coordinate system westward about the poles of the ecliptic, completing one circuit in about 26,000 years. Superimposed on this is a smaller motion of the ecliptic, and a small oscillation of the Earth's axis, nutation. Explanatory Supplement (1961), pp. 20, 28 In order to reference a coordinate system which can be considered as fixed in space, these motions require specification of the equinox of a particular date, known as an epoch, when giving a position in ecliptic coordinates.
As seen from the orbiting Earth, the Sun appears to move with respect to the fixed stars, and the ecliptic is the yearly path the Sun follows on the celestial sphere. This process repeats itself in a cycle lasting a little over 365 days. The ecliptic is the plane of Earth's orbit around the Sun. From the perspective of an observer on Earth, the Sun's movement around the celestial sphere over the course of a year traces out a path along the ecliptic against the background of stars.
The plane of Earth's orbit projected in all directions forms the reference plane known as the ecliptic. Here, it is shown projected outward (gray) to the celestial sphere, along with Earth's equator and polar axis (green). The plane of the ecliptic intersects the celestial sphere along a great circle (black), the same circle on which the Sun seems to move as Earth orbits it. The intersections of the ecliptic and the equator on the celestial sphere are the vernal and autumnal equinoxes (red), where the Sun seems to cross the celestial equator.
Because the orbit of the Moon is inclined only about 5.145° to the ecliptic and the Sun is always very near the ecliptic, eclipses always occur on or near it. Because of the inclination of the Moon's orbit, eclipses do not occur at every conjunction and opposition of the Sun and Moon, but only when the Moon is near an ascending or descending node at the same time it is at conjunction (new) or opposition (full). The ecliptic is so named because the ancients noted that eclipses only occur when the Moon is crossing it.
It gave a concurring period of 6.01375 hours and two spin axis in ecliptic coordinates of (184.0°, −43.0°) and (353.0°, −17.0°).
The nodal cycle is found to be about 600 years, within which occur two ecliptic phases, each lasting about 100 yr.
It gave a sidereal period of and two spin axes at (94.0°, −25.0°) and (269.0°, 4.0°) in ecliptic coordinates (λ, β).
It is a slow rotator and potentially a tumbler as well. The object was probably ejected from the ecliptic by Neptune.
The conjunctions in right ascension occur in a coordinate system measured by a set of coordinates based on the celestial equator. This great circle is a projection of the Earth's equator into the sky. The second system is based on the ecliptic, the plane of the Solar System. When measured along the ecliptic, the separations are usually smaller.
The correction is zero (HJD = JD) for objects at the poles of the ecliptic. Elsewhere, it is approximately an annual sine curve, and the highest amplitude occurs on the ecliptic. The maximum correction corresponds to the time in which light travels the distance from the Sun to the Earth, i.e. ±8.3 min (500 s, 0.0058 days).
It gave a concurring sidereal period of hours and includes a partial spin axis at (β1 −53.0°) in ecliptic coordinates (λ, β).
Al- Biruni reports that his work on the ecliptic was carried out in Shiraz. He lived at the Buyid court in Isfahan.
Nakshatras are divisions of ecliptic, each 13° 20', starting from 0° Aries. The purnima of each month is synchronised with a nakshatra.
It showed a sidereal period of hours (), and gave two spin axes at (18.0°, 4.0°) and (192.0°, 32.0°) in ecliptic coordinates (λ, β).
The Surtian orbit is retrograde, at an inclination of 166.9° to the ecliptic (148.9° to Saturn's equator) and with an eccentricity of 0.3680.
The Great Year, or equinoctial cycle, corresponds to a complete revolution of the equinoxes around the ecliptic. Its length is about 25,700 years.
In addition to the steady progressive motion (resulting in a full circle in about 25,700 years) the Sun and Moon also cause small periodic variations, due to their changing positions. These oscillations, in both precessional speed and axial tilt, are known as the nutation. The most important term has a period of 18.6 years and an amplitude of 9.2 arcseconds. In addition to lunisolar precession, the actions of the other planets of the Solar System cause the whole ecliptic to rotate slowly around an axis which has an ecliptic longitude of about 174° measured on the instantaneous ecliptic.
Gauchet, 151. Along with a later 17th-century Chinese illustration of Guo's mathematical proofs, Needham states that: : Guo used a quadrangular spherical pyramid, the basal quadrilateral of which consisted of one equatorial and one ecliptic arc, together with two meridian arcs, one of which passed through the summer solstice point...By such methods he was able to obtain the du lü (degrees of equator corresponding to degrees of ecliptic), the ji cha (values of chords for given ecliptic arcs), and the cha lü (difference between chords of arcs differing by 1 degree).Needham, Volume 3, 109–110.
Because Earth's rotational axis is not perpendicular to its orbital plane, Earth's equatorial plane is not coplanar with the ecliptic plane, but is inclined to it by an angle of about 23.4°, which is known as the obliquity of the ecliptic.Explanatory Supplement (1992), p. 733 If the equator is projected outward to the celestial sphere, forming the celestial equator, it crosses the ecliptic at two points known as the equinoxes. The Sun, in its apparent motion along the ecliptic, crosses the celestial equator at these points, one from south to north, the other from north to south.
In the Solar System, the planets and the Sun lie roughly within the same flat plane, known as the plane of the ecliptic. From our perspective on Earth, the ecliptic is the path taken by the Sun across the sky over the course of the year. The twelve constellations that line the ecliptic are known as the zodiacal constellations, and, annually, the Sun passes through all of them in turn. Additionally, over time, the Sun's annual cycle appears to recede very slowly backward by one degree every 72 years, or by one constellation approximately every 2,160 years.
The orbit of Camillo is highly inclined. Vertical lines show the distance above and below the ecliptic every 30 days. Camillo orbits the Sun at a distance of 0.99–1.8 AU once every 20 months (614 days; semi-major axis of 1.41 AU). Its orbit has an eccentricity of 0.30 and an inclination of 56° with respect to the ecliptic.
As the region of sky close to the ecliptic became well explored, later sky surveys began looking for objects that had been dynamically excited into orbits with higher inclinations, as well as more distant objects, with slower mean motions across the sky. These surveys eventually covered the location of Haumea, with its high orbital inclination and current position far from the ecliptic.
From antiquity through the 18th century, ecliptic longitude was commonly measured using twelve zodiacal signs, each of 30° longitude, a practice that continues in modern astrology. The signs approximately corresponded to the constellations crossed by the ecliptic. Longitudes were specified in signs, degrees, minutes, and seconds. For example, a longitude of is 19.933° east of the start of the sign Leo.
The dust band that causes the zodiacal light is uniform across the whole ecliptic. The dust further from the ecliptic is almost undetectable except when viewed at a small angle with the sun. Thus it is possible to see more of the width at small angles toward the sun, and it appears wider near the horizon, closer to the sun under the horizon.
Throughout the year the star will rise approximately four minutes earlier each successive sunrise. Eventually the star will return to its same relative location at sunrise. This length of time can be called an observational year. Stars that reside close to the ecliptic or the ecliptic meridian will on average exhibit observational years close to the sidereal year of 365.2564 days.
It gave a concurring period of hours, as well as two spin axes at (3.0°, −81.0°) and (183.0°, −72.0°) in ecliptic coordinates (λ, β).
Modelling gave a concurring sidereal rotation period of hours, as well as two spin axes of (132.0°, −46.0°) and (305.0°, −49.0°) in ecliptic coordinates.
It gave a concurring period of hours, as well as two spin axes at (52.0°, −51.0°) and (235.0°, −43.0°) in ecliptic coordinates (λ, β).
It gave a concurring sidereal period of hours and includes two spin axes at (119.0°, 7.0°) and (301.0°, 5.0°) in ecliptic coordinates (λ, β).
Conformations of ferrocene. Left: staggered; right: ecliptic. An important parameter is the angle between the two cyclopentadienyl ligands. Often the reactivity increases with increasing angle.
It gave a sidereal period of 20.9959 hours, as well as a spin axis in ecliptic coordinates (λ, β) of (326.0°, 37.0°) and (144.0°, 79.0°).
A 2016 paper reports that the trapezoid rule was in use in Babylon before 50 BCE for integrating the velocity of Jupiter along the ecliptic.
It gave a concurring period of 16.1894 hours, as well as two spin axes at (352.0°, −18.0°) and (173.0°, −32.0°) in ecliptic coordinates (λ, β).
Lightcurve inversion gave a concurring period of hours, as well as two spin axes of (16.0°, 59.0°) and (209.0°, 50.0°) in ecliptic coordinates (λ, β).
They gave a period of 10.42466 and 10.42468 hours, as well as a spin axis of (0°, 71.0°) and (251.0°, 75.0°) in ecliptic coordinates, respectively.
On average, orbits about 81 AU from the Sun, taking approximately 727 years to complete one full orbit around the Sun. With an orbital eccentricity of about 0.53, it follows a highly elongated orbit, varying in distance from 37.8 AU at perihelion to 123.8 AU at aphelion. Its orbit is inclined to the ecliptic plane by 24.5 degrees, with its aphelion oriented below the ecliptic.
Croswell (1997), p. 43. Lowell's first search focused on the ecliptic, the plane encompassed by the zodiac where the other planets in the Solar System lie. Using a 5-inch photographic camera, he manually examined over 200 three-hour exposures with a magnifying glass, and found no planets. At that time Pluto was too far above the ecliptic to be imaged by the survey.
The ecliptic forms the center of the zodiac, a celestial belt about 20° wide in latitude through which the Sun, Moon, and planets always appear to move. Traditionally, this region is divided into 12 signs of 30° longitude, each of which approximates the Sun's motion in one month.Bryant (1907), p. 4. In ancient times, the signs corresponded roughly to 12 of the constellations that straddle the ecliptic.
Coma Ecliptic is the seventh studio album by American progressive metal band Between the Buried and Me, released on July 10, 2015 through Metal Blade Records. The band first announced the album through Twitter on September 8, 2014 saying "It has begun! #rockopera". Similar to previous releases by the band, Coma Ecliptic is a concept album. The first single, "Memory Palace" was released on April 3, 2015.
M2 and M6 The crossing from north to south is the autumnal equinox or descending node. The orientation of Earth's axis and equator are not fixed in space, but rotate about the poles of the ecliptic with a period of about 26,000 years, a process known as lunisolar precession, as it is due mostly to the gravitational effect of the Moon and Sun on Earth's equatorial bulge. Likewise, the ecliptic itself is not fixed. The gravitational perturbations of the other bodies of the Solar System cause a much smaller motion of the plane of Earth's orbit, and hence of the ecliptic, known as planetary precession.
The mean inclination of the lunar orbit to the ecliptic plane is 5.145°. Theoretical considerations show that the present inclination relative to the ecliptic plane arose by tidal evolution from an earlier near-Earth orbit with a fairly constant inclination relative to Earth's equator. It would require an inclination of this earlier orbit of about 10° to the equator to produce a present inclination of 5° to the ecliptic. It is thought that originally the inclination to the equator was near zero, but it could have been increased to 10° through the influence of planetesimals passing near the Moon while falling to the Earth.
After a stint at NASA, he returned to help attract in 1981 the Space Telescope Science Institute to JHU, an organization that now employs 500, including 100 PhDs. More recently he has attracted popular press for the SETI ecliptic search idea, and the Hanke-Henry Permanent Calendar. The SETI ecliptic search idea suggests focusing SETI efforts in the ecliptic plane in which distant hypothetical observers can see the Earth's transit of the sun. The Hanke-Henry Permanent Calendar is one in which the number of days in a year is always divisible by seven, such that holidays always fall on the same day of the week.
Its orbit has an eccentricity of 0.06 and an inclination of 28° with respect to the ecliptic. Its inclination is almost as high as that of .
This yielded a sidereal rotation period of . They found two possible solutions for the spin axis, with the preferred solution in ecliptic coordinates being (λ, β) = (, ).
It gave a concurring sidereal period of 7.87149 hours, as well as two spin axes of (7.0°, 55.0°) and (170.0°, 65.0°) in ecliptic coordinates (λ, β).
Where the obliquity of the ecliptic is not obtained elsewhere, it can be approximated: : \epsilon = 23.439^\circ - 0.0000004^\circ n for use with the above equations.
Dorado is also the location of the South Ecliptic pole, which lies near the fish's head. The pole was called "Polus Doradinalis" by Willem Jansson Blaeu.
Analysis of 2015 radar observations obtained at the Arecibo Observatory and the Goldstone Observatory yields a spin axis of (270.0°, −81.0°) in ecliptic coordinates (λ, β).
NGC 6543 is 4.4 minutes of arc from the current position of the north ecliptic pole, less than of the 45 arc minutes between Polaris and the current location of the Earth's northern axis of rotation. It is a convenient and accurate marker for the axis of rotation of the Earth's ecliptic, around which the celestial North Pole rotates. It is also a good marker for the nearby “invariable” axis of the solar system, which is the center of the circles which every planet's north pole, and the north pole of every planet's orbit, make in the sky. Since motion in the sky of the ecliptic pole is very slow compared to the motion of the Earth's north pole, its position as an ecliptic pole station marker is essentially permanent on the time-scale of human history, as opposed to the Pole Star, which changes every few thousand years.
While its aphelion is outside that of Jupiter's orbit, it is so highly inclined that its furthest point from the Sun is far out of the ecliptic.
In 2013, an international study modeled a lightcurve with a period of 14.0591 hours and found a spin axis of (5.0°, 80.0°) in ecliptic coordinates (λ, β) ().
Most recent results gave a concurring sidereal period of hours, as well as two spin axes at (325.0°, 35.0°) and (137.0°, 66.0°) in ecliptic coordinates (λ, β).
It gave a concurring sidereal period of and hours, respectively. Hanuš also gave two spin axes at (235.0°, −52.0°) and (47.0°, 84.0°) in ecliptic coordinates (λ, β).
The upper portion is now set at an angle equal to the obliquity of the ecliptic, which allows the instrument to give ecliptic coordinates. This measures the celestial bodies now on celestial latitude and longitude scales which allow for greater precision and accuracy in making measurements. These three differing configurations allowed for added convenience in taking readings and made once tedious and complicated measuring more streamlined and simple.
Quasi-satellite orbit of in the year 2589, looking vertically down on the ecliptic. Left, orbits of Asteroid and Earth in the reference frame of the fixed stars; right, in the reference frame of the Earth–Sun system. Image: JPL Because of its orbital inclination of 10.739° to the ecliptic, is not always forced by the Earth on its horseshoe orbit however but can sometimes slip out of this pattern.
This description of the orientation of the reference frame is somewhat simplified; the orientation is not quite fixed. A slow motion of Earth's axis, precession, causes a slow, continuous turning of the coordinate system westward about the poles of the ecliptic, completing one circuit in about 26,000 years. Superimposed on this is a smaller motion of the ecliptic, and a small oscillation of the Earth's axis, nutation.Explanatory Supplement (1961), pp.
The plane of reference can be aligned with the Earth's celestial equator, the ecliptic, or the Milky Way's galactic equator. These 3D celestial coordinate systems add actual distance as the Z axis to the equatorial, ecliptic, and galactic coordinate systems used in spherical astronomy. The distances involved are so great compared to the relative velocities of the stars, that for most purposes, the time component can be neglected.
In 2013, another modeled lightcurve obtained form photometric data collected by the Catalina Sky Survey also determined a spin axis of (334.0°, −84.0°) in ecliptic coordinates (λ, β).
In 2016, a modeled lightcurve gave a concurring period of 7.33200 hours and determined two spin axis of (124.0°, 32.0°) and (322.0°, 60.0°) in ecliptic coordinates (λ, β).
ArcLight is a genetically-encoded voltage indicator (GEVI) created from Ciona intestinalis voltage sensor and the fluorescent protein super ecliptic pHluorin that carries a critical point mutation (A227D).
The three most commonly used are: ;Mean equinox of a standard epoch: (usually the J2000.0 epoch, but may include B1950.0, B1900.0, etc.) is a fixed standard direction, allowing positions established at various dates to be compared directly. ;Mean equinox of date: is the intersection of the ecliptic of "date" (that is, the ecliptic in its position at "date") with the mean equator (that is, the equator rotated by precession to its position at "date", but free from the small periodic oscillations of nutation). Commonly used in planetary orbit calculation. ;True equinox of date: is the intersection of the ecliptic of "date" with the true equator (that is, the mean equator plus nutation).
Astronomically, the zodiac defines a belt of space extending 9° either side of the ecliptic, within which the orbits of the Moon and the principal planets remain. It is a feature of a celestial coordinate system centered upon the ecliptic, (the plane of the Earth's orbit and the Sun's apparent path), by which celestial longitude is measured in degrees east of the vernal equinox (the ascending intersection of the ecliptic and equator). Stars within the zodiac are subject to occultations by the Moon and other solar system bodies. These events can be useful, for example, to estimate the cross-sectional dimensions of a minor planet, or check a star for a close companion.
The 12 months came about by dividing the ecliptic into 12 equal segments of 30 degrees and were given zodiacal constellation names which was later used by the Greeks.
Eratosthenes most probably used a solstitial armilla for measuring the obliquity of the ecliptic. Hipparchus probably used an armillary sphere of four rings.Editors of Encyclopædia Britannica. (16 November 2006).
In 2016, an international study modeled a lightcurve with a period of hours and found two spin axes of (51.0°, 76.0°) and (275.0°, 58.0°) in ecliptic coordinates (λ, β).
As seen from Mars, the ecliptic (apparent plane of the sun and also the average plane of the planets which is almost the same) passes into Cetus - the centre of the sun is a foreground object in Cetus for around six days shortly after the northern summer solstice. Mars's orbit is tilted by 1.85° with respect to Earth's - Mars has relatively great 'inclination', that is, is marginally inclined away from the ecliptic.
Bardwell is a member of the Themis family, a dynamical family of outer-belt asteroids with nearly coplanar ecliptical orbits. It orbits the Sun at a distance of 2.6–3.7 AU once every 5 years and 6 months (2,020 days). Its orbit has an eccentricity of 0.18 and an inclination of 2° with respect to the ecliptic. Its orbit has an eccentricity of 0.18 and an inclination of 2° with respect to the ecliptic.
Buffy was discovered on 11 December 2004. It was discovered by astronomers led by (Rhiannon) Lynne Allen of the University of British Columbia as part of the Canada–France Ecliptic Plane Survey (CFEPS) using the Canada–France–Hawaii Telescope (CFHT) near the ecliptic. The team included Brett Gladman, John Kavelaars, Jean-Marc Petit, Joel Parker and Phil Nicholson. In 2015, six precovery images from 2002 and 2003 were found in Sloan Digital Sky Survey data.
The asteroid's lightcurve has also been modeled twice. In 2011, the first modelling used photometric data from the AstDyS database and the Uppsala Asteroid Photometric Catalogue, and found two spin axis of (248.0°, −68.0°) and (83.0°, −66.0°) in ecliptic coordinates (λ, β). A refined modeling in 2016, using the Lowell Photometric Database gave two poles of (50.0°, −65.0°) and (233.0°, −68.0°) in ecliptic coordinates. Also, both studies found a concurring period of 5.35059 hours.
Those manoeuvres were to reach other planets also orbiting close to the ecliptic, so they were mostly in-plane changes. However, gravity assists are not limited to in-plane maneuvers; a suitable flyby of Jupiter could produce a significant plane change. An Out-Of-The-Ecliptic mission (OOE) was thereby proposed. See article Pioneer H. Originally, two spacecraft were to be built by NASA and ESA, as the International Solar Polar Mission.
Its orbit has an eccentricity of 0.07 and an inclination of 8° with respect to the ecliptic. As no precoveries were taken, the asteroid's observation arc begins with its discovery.
In 2016, a modeled lightcurve using photometric data from various sources gave a concurring period of hours and two spin axis of (222.0°, −66°) and (40.0°, −77.0°) in ecliptic coordinates.
In 2016, an international study modeled a lightcurve with a concurring period of hours and found two spin axes of (269.0°, −31.0°) and (103.0°, −59.0°) in ecliptic coordinates (λ, β) ().
Its orbit has an eccentricity of 0.52 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its official discovery observation in July 2010.
38083 Rhadamanthus is a trans-Neptunian object (TNO). It was discovered in 1999 by the Deep Ecliptic Survey. It was originally thought to be a plutino but no longer is.
Burnam's Celestial Handbook, pp. 1107-1108. Due to its position on the ecliptic, it is sometimes obscured by the Moon or planets. A lunar occultation took place April 4, 2012.
As seen from Earth, the Sun moves from west to east along the ecliptic, passing over the course of one year through the twelve constellations of the Zodiac, and Ophiuchus.
In 2013, an international study modeled a lightcurve with a sidereal period of 8.82653 hours and found two spin axes at (47.0°, 57.0°) and (234.0°, 50.0°) in ecliptic coordinates (λ, β) ().
In 2016, an international study modeled a lightcurve with a concurring period of 216.98 hours and found two spin axis of (314.0°, −46.0°) and (107.0°, −56.0°) in ecliptic coordinates (λ, β).
In 2013, an international study modeled a lightcurve with a similar period of 4.30435 hours and found two spin axis of (275.0°, 29.0°) and (94.0°, 33.0°) in ecliptic coordinates (λ, β) .
In 2013, an international study modeled a lightcurve with a concurring period of 15.0276 hours and found two spin axis of (252.0°, 51.0°) and (64.0°, 41.0°) in ecliptic coordinates (λ, β) ().
Its orbit has an eccentricity of 0.10 and an inclination of 7° with respect to the ecliptic. Its observation arc begins with its official discovery observation at Palomar in September 1960.
Its orbit has an eccentricity of 0.11 and an inclination of 2° with respect to the ecliptic. The body's observation arc begins 15 days after its official discovery observation at Heidelberg.
In 2013, an international study modeled a lightcurve with a concurring period of 10.6590 hours and found a spin axis of (266.0°, 67.0°) and (62.0°, 67.0°) in ecliptic coordinates (λ, β) ().
In 2013, an international study modeled a lightcurve with a concurring period of 9.15751 hours and found two spin axis of (282.0°, 44.0°) and (86.0°, 42.0°) in ecliptic coordinates (λ, β) ().
The alignment of the axis is maintained throughout the year so that the point of sky above the north or south poles remains unchanged throughout the Earth's annual rotation around the Sun. A slow conical motion of the Earth's polar axis about its normal to the plane of the ecliptic is caused by the attractive force of the other heavenly bodies on the equatorial protuberance of the Earth. A similar conical motion can also be observed in a gyroscope that is subjected to lateral forces. The resultant motion of the Earth's axis is called general precession and the equinox points in the ecliptic move westward along the ecliptic at the rate of about 50.3 seconds of arc per year as a result.
It is customary to specify positions of celestial bodies with respect to the vernal equinox. Because of Earth's precession of the equinoxes, this point moves back slowly along the ecliptic. Therefore, it takes the Moon less time to return to an ecliptic longitude of 0° than to the same point amid the fixed stars: days (27 d 7 h 43 m 4.7 s). This slightly shorter period is known as the tropical month; compare the analogous tropical year.
Planets orbiting the Sun follow elliptical (oval) orbits that rotate gradually over time (apsidal precession). The eccentricity of this ellipse, as well as the rate of precession, is exaggerated for visualization. In addition, the orbital ellipse itself precesses in space, in an irregular fashion, completing a full cycle every 112,000 years relative to the fixed stars. Apsidal precession occurs in the plane of the ecliptic and alters the orientation of the Earth's orbit relative to the ecliptic.
Because the signs are each 30° in longitude but constellations have irregular shapes, and because of precession, they do not correspond exactly to the boundaries of the constellations after which they are named. These astrological signs form a celestial coordinate system, or even more specifically an ecliptic coordinate system, which takes the ecliptic as the origin of latitude and the Sun's position at vernal equinox as the origin of longitude.; numerous examples of this notation appear throughout the book.
Because the division was made into equal arcs, 30° each, they constituted an ideal system of reference for making predictions about a planet's longitude. However, Babylonian techniques of observational measurements were in a rudimentary stage of evolution.Sachs (1948), p. 289. They measured the position of a planet in reference to a set of "normal stars" close to the ecliptic (±9° of latitude) as observational reference points to help positioning a planet within this ecliptic coordinate system.
As planning for the Pioneer 10 and 11 missions progressed, mission scientists found themselves desiring a third probe. In 1971, a formal mission study was proposed for a spacecraft to be launched to Jupiter in 1974, where it would use the gas giant as a gravitational slingshot to travel outside the ecliptic. This was the first Out-Of-The-Ecliptic mission (OOE) proposed, for Jupiter and solar (Sun) observations. NASA/Ames Research Center would have managed the project.
Its orbit has an eccentricity of 0.05 and an inclination of 26° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Palomar in August 1988.
Its orbit has an eccentricity of 0.09 and an inclination of 22° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Palomar in March 1971.
In addition a modeled lightcurve, using photometric data from various sources, gave a concurring period of 9.45950 hours and determined two spin axis of (356.0°, −58.0°) and (233.0°, −89.0°) in ecliptic coordinates.
In 2016, an international study modeled a lightcurve with a concurring period of 9.19182 hours. It also determined two spin axis at (352.0°, 72.0°) and (166.0°, 73.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.09 and an inclination of 9° with respect to the ecliptic. The body's observation arc begins at Palomar with its official discovery observation in September 1988.
In 2016, a modeled lightcurve using photometric data from various sources, rendered a similar sidereal period of 12.15186 hours and two spin axes of (32.0°, 22.0°) and (216.0°, 55.0°) in ecliptic coordinates.
Its orbit has an eccentricity of 0.19 and an inclination of 17° with respect to the ecliptic. The body's observation arc begins at Algiers on its official discovery observation in January 1925.
In 2013, an international study modeled a lightcurve with a concurring period of 4.97347 hours and found a spin axis of (44.0°, 59.0°) and (222.0°, 68.0°) in ecliptic coordinates (λ, β), respectively ().
Pluto was easiest to find because it has the highest apparent magnitude of all known trans-Neptunian objects. It also has a lower inclination to the ecliptic than most other large TNOs.
The difference between reference to an epoch alone, and a reference to a certain equinox with equator or ecliptic, is therefore that the reference to the epoch contributes to specifying the date of the values of astronomical variables themselves; while the reference to an equinox along with equator/ecliptic, of a certain date, addresses the identification of, or changes in, the coordinate system in terms of which those astronomical variables are expressed. (Sometimes the word 'equinox' may be used alone, e.g. where it is obvious from the context to users of the data in which form the considered astronomical variables are expressed, in equatorial form or ecliptic form.) The equinox with equator/ecliptic of a given date defines which coordinate system is used. Most standard coordinates in use today refer to 2000 TT (i.e. to 12h on the Terrestrial Time scale on January 1, 2000), which occurred about 64 seconds sooner than noon UT1 on the same date (see ΔT). Before about 1984, coordinate systems dated to 1950 or 1900 were commonly used.
A scheme introduced by a 2005 report from the Deep Ecliptic Survey by J. L. Elliott et al. distinguishes between two categories: scattered-near (i.e. typical SDOs) and scattered- extended (i.e. detached objects).
Its orbit has an eccentricity of 0.07 and an inclination of 23° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at La Silla in February 1994.
Therefore, both the normal to the orbital plane and the Moon's rotational axis precess around the ecliptic pole with the same period. The period is about 18.6 years and the motion is retrograde.
A heliacal year is the interval between the heliacal risings of a star. It differs from the sidereal year for stars away from the ecliptic due mainly to the precession of the equinoxes.
Its orbit has an eccentricity of 0.08 and an inclination of 27.4° with respect to the ecliptic. This object has the second highest inclination of any known Neptune trojan after , which has 29.3°.
Polar and ecliptic view of the orbit of Varda. Varda was discovered in March 2006, using imagery dated from 21 June 2003 by Jeffrey A. Larsen with the Spacewatch telescope as part of a United States Naval Academy Trident Scholar project. It orbits the Sun at a distance of 39.5–52.7 AU once every 313.1 years (over 114,000 days; semi-major axis of 46.1 AU). Its orbit has an eccentricity of 0.14 and an inclination of 21.5° with respect to the ecliptic.
Astronomical dial Inside the large black outer circle lies another movable circle marked with the signs of the zodiac which indicates the location of the Sun on the ecliptic. The signs are shown in anticlockwise order. In the photograph accompanying this section, the Sun is currently moving anticlockwise from Cancer into Leo. The displacement of the zodiac circle results from the use of a stereographic projection of the ecliptic plane using the North pole as the basis of the projection.
Hatshepsut is a member of the Hygiea family (), a very large family of carbonaceous outer-belt asteroids, named after the fourth-largest asteroid, 10 Hygiea. It orbits the Sun in the outer main-belt at a distance of 2.9–3.5 AU once every 5 years and 8 months (2,072 days). Its orbit has an eccentricity of 0.10 and an inclination of 4° with respect to the ecliptic. Its orbit is only slightly eccentric and not much inclined to the ecliptic.
The true solar day tends to be longer near perihelion when the Sun apparently moves along the ecliptic through a greater angle than usual, taking about longer to do so. Conversely, it is about shorter near aphelion. It is about longer near a solstice when the projection of the Sun's apparent motion along the ecliptic onto the celestial equator causes the Sun to move through a greater angle than usual. Conversely, near an equinox the projection onto the equator is shorter by about .
B. L. van der Waerden, "History of the zodiac", Archiv für Orientforschung 16 (1953) 216–230. The term "zodiac" may also refer to the region of the celestial sphere encompassing the paths of the planets corresponding to the band of about 8 arc degrees above and below the ecliptic. The zodiac of a given planet is the band that contains the path of that particular body; e.g., the "zodiac of the Moon" is the band of 5° above and below the ecliptic.
Its orbit has an eccentricity of 0.18 and an inclination of 3° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory with its official discovery observation on 8 September 1915.
A modeled lightcurve derived from combined dense and sparse photometric data was published in 2013. It gave a concurring period of hours and a spin axis at (78.0°, −82.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.04 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins at Heidelberg in March 1924, six days after its official discovery observation.
Information on sky watching in all seasons, plus sky photos and star charts. There is also information on light pollution, the Ecliptic and the Zodiac plus reality checks of the urban myths of stargazing.
It orbits the Sun at a distance of 0.9–2.2 AU once every 23 months (708 days). Its orbit has an eccentricity of 0.44 and an inclination of 6° with respect to the ecliptic.
This is located roughly midway between Delta Draconis and Zeta Draconis. The north ecliptic pole almost coincides with the south celestial pole of Venus; Zeta Draconis is also the north pole star of Jupiter.
Officially discovered on 31 May 2008, the discovery was announced on 16 July 2008, by the Canada–France Ecliptic Plane Survey team led by Brett Gladman. The discovery team nicknamed "Drac" after Count Dracula.
The Ab1 component's unseen companion, Beta Capricorni Ab2, orbits Ab1 with an orbital period of 8.7 days. Beta¹ Capricorni is 4.6 degrees north of the ecliptic, so it can be occulted by the Moon.
In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a period hours, as well as a spin axis of (22.0°, 76.0°) in ecliptic coordinates (λ, β) ().
Its orbit has an eccentricity of 0.28 and an inclination of 3.4° with respect to the ecliptic. The body's observation arc begins with its first observation at the Siding Spring Observatory on 21 August 2006.
Another production was the Horæ Mathematicæ Vacuæ, a treatise on Golden and Ecliptic Numbers (1743), written as a pastime during an attack of sciatica; the manuscript of this work was preserved in Sion College Library.
In 2013, an international study also modeled the asteroid's lightcurve from photometric data. It gave a concurring period of 4.10295 hours and determined a partial spin axis of (n.a., 47.0°) in ecliptic coordinates (λ, β).
The orbit of Pallas was determined by Gauss, who found the period of 4.6 years was similar to the period for Ceres. Pallas has a relatively high orbital inclination to the plane of the ecliptic.
In 2016, an international study modeled a lightcurve from various data sources with a period of 17.5611 hours and found two spin axis of (86.0°, −65.0°) and (272.0°, −42.0°), respectively, in ecliptic coordinates (λ, β) ().
The Gemini that worked for Ecliptic was actually two people. One of the Geminis was actually Madison Jeffries who was brainwashed into serving the Zodiac. The two Geminis spoke as one when they are together.
Lightcurve analysis indicates that Alice's pole points towards either ecliptic coordinates (β, λ) = (55°, 65°) or (β, λ) = (55°, 245°) with a 10° uncertainty. This gives an axial tilt of about 35° in both cases.
A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database (LPD), gave a concurring period of 7.14117 hours, as well as a spin axis of (40.0°, 43.0°) in ecliptic coordinates (λ, β).
Also known as the Axial system, or Equatorial system, it divides the celestial equator in twelve 30° sectors (starting at the local meridian) and projects them on to the ecliptic along the great circles containing the North and South celestial poles. The intersections of the ecliptic with those great circles provide the house cusps. The 10th house cusp thus equals the Midheaven, but the East Point (also known as Equatorial Ascendant) is now the first house's cusp. Each house is exactly 2 sidereal hours long.
Its orbit has an eccentricity of 0.17 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 11 October 1920, the night after its official discovery observation.
Its eccentric orbit of 0.26 is inclined by 11 degrees towards the plane of the ecliptic. Kaisers observation arc begins with its official discovery observation, as no precoveries were taken, and no prior identifications were made.
A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database, gave a concurring period of 15.6873 hours and determined two spin axis in ecliptic coordinates (λ, β) of (153.0°, 32.0°) and (314.0°, 46.0°).
In 2016, the asteroid lightcurve has also been modeled using photometric data from various sources. It gave a concurring period of 16.1834 hours and two spin axis in ecliptic coordinates of (352.0°, 49.0°) and (201.0°, 55.0°).
"Glossary" in Astronomical Almanac Online. (2018). Washington DC: United States Naval Observatory. s.v. obliquity. This value remains about the same relative to a stationary orbital plane throughout the cycles of axial precession. But the ecliptic (i.e.
Its orbit has an eccentricity of 0.29 and an inclination of 4° with respect to the ecliptic. Wild observation arc begins with its discovery observation, as , a previous identification made at Heidelberg in 1918, remained unused.
166 (2003), pp. 33-45 The satellite orbits Jupiter at an average distance of 21,064,000 km in 624.542 days, at an inclination of 147° to the ecliptic (147° to Jupiter's equator) with an eccentricity of 0.2441.
This section refers to labels in the diagram below. (Open it in a second window on your screen for easy magnified reference.) Armillary sphere diagram The exterior parts of this machine are a compages [or framework] of brass rings, which represent the principal circles of the heavens. # The equinoctial A, which is divided into 360 degrees (beginning at its intersection with the ecliptic in Aries) for showing the sun's right ascension in degrees; and also into 24 hours, for showing its right ascension in time. # The ecliptic B, which is divided into 12 signs, and each sign into 30 degrees, and also into the months and days of the year; in such a manner, that the degree or point of the ecliptic in which the sun is, on any given day, stands over that day in the circle of months.
The year is usually represented by the 12 signs of the zodiac, arranged either as a concentric circle inside the 24-hour dial, or drawn onto a displaced smaller circle, which is a projection of the ecliptic, the path of the sun and planets through the sky, and the plane of the Earth's orbit. The ecliptic plane is projected onto the face of the clock, and, because of the Earth's tilted angle of rotation relative to its orbital plane, it is displaced from the center and appears to be distorted. The projection point for the stereographic projection is the North pole; on astrolabes the South pole is more common. The ecliptic dial makes one complete revolution in 23 hours 56 minutes (a sidereal day), and will therefore gradually get out of phase with the hour hand, drifting slowly further apart during the year.
A modeled lightcurve using photometric data from the Lowell Photometric Database was published in 2016. It gave a sidereal period of 42.8982 hours, as well as a spin axis at (352.0°, −66.0°) in ecliptic coordinates (λ, β).
The value of in the above calculation is an accurate value for the Sun's ecliptic longitude (shifted by 90°), so the solar declination becomes readily available: :Declination = which is accurate to within a fraction of a degree.
Mendoza orbits the Sun at a distance of 2.1–2.6 AU once every 3 years and 7 months (1,302 days). Its orbit has an eccentricity of 0.10 and an inclination of 8° with respect to the ecliptic.
It orbits the Sun at a distance of 2.3–3.3 AU once every 4 years and 8 months (1,697 days). Its orbit has an eccentricity of 0.19 and an inclination of 7° with respect to the ecliptic.
A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database, gave a concurring period of 7.30136 hours, as well as two spin axis of (92.0°, −69.0°) and (256.0°, −76.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.14 and an inclination of 3° with respect to the ecliptic. The body's observation arc begins at Heidelberg in January 1951, or more than 24 years after its official discovery observation.
A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database (LPD), gave a concurring period of hours, as well as two spin axes of (78.0°, −50.0°) and (267.0°, −51.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.04 and an inclination of 21° with respect to the ecliptic. Vyssotskys observation arc begins with its official discovery observation, as no precoveries were taken, and no prior identifications were made.
Lutetia orbits the Sun at the distance of approximately 2.4 AU in the inner asteroid belt. Its orbit lies almost in the plane of ecliptic and is moderately eccentric. The orbital period of Lutetia is 3.8 years.
Metsähovi orbits the Sun at a distance of 2.1–2.4 AU once every 3 years and 5 months (1,248 days). Its orbit has an eccentricity of 0.08 and an inclination of 8° with respect to the ecliptic.
NGC 840 is a barred spiral galaxy in the constellation Cetus south of the ecliptic. It is estimated to be about 300 million light-years from the Milky Way and has a diameter of approximately 175,000 ly.
They gave a concurring sidereal period of 11.3981 and 11.39823 hours, respectively. Each study also determined two respective spin axes of (79.0°, 75.0°) and (282.0°, 55.0°), and (71.0°, 61.0°) and (280.0°, 54.0°) in ecliptic coordinates (λ, β).
The irregular daily movement of the Sun was known to the Babylonians. Book III of Ptolemy's Almagest (2nd century) is primarily concerned with the Sun's anomaly, and he tabulated the equation of time in his Handy Tables. Ptolemy discusses the correction needed to convert the meridian crossing of the Sun to mean solar time and takes into consideration the nonuniform motion of the Sun along the ecliptic and the meridian correction for the Sun's ecliptic longitude. He states the maximum correction is time-degrees or of an hour (Book III, chapter 9).
Other members of the network include or have included the Indian SROSS-C2 spacecraft, the US Air Force's Defense Meteorological Satellites, the Japanese Yohkoh spacecraft, and the Chinese SZ-2 mission. These have all been Earth orbiters, and the Chinese and Indian detectors were operational for only a few months. Of all the above, Ulysses is the only spacecraft whose orbit takes it large distances away from the ecliptic plane. These deviations from the ecliptic plane allow more precise 3-D measurements of the apparent positions of the GRBs.
Orcus is in a 2:3 orbital resonance with Neptune, having an orbital period of 245 years, and is classified as a plutino. Its orbit is moderately inclined at 20.6 degrees to the ecliptic. Orcus's orbit is similar to Pluto's (both have perihelia above the ecliptic), but is oriented differently. Although at one point its orbit approaches that of Neptune, the resonance between the two bodies means that Orcus itself is always a great distance away from Neptune (there is always an angular separation of over 60 degrees between them).
The equinoxes move westward along the ecliptic relative to the fixed stars, opposite to the yearly motion of the Sun along the ecliptic, returning to the same position approximately every 26,000 years. The "Serpent Numbers" in the Dresden codex pp. 61–69 is a table of dates written in the coils of undulating serpents. Beyer was the first to notice that the Serpent Series is based on an unusually long distance number of 1.18.1.8.0.16 (5,482,096 days – more than 30,000 years).Beyer, Hermann 1943 Emendations of the ‘Serpent Numbers’ of the Dresden Maya Codex.
Sausalito: University Science Books. p. 99. This is similar to the precession of a spinning-top, with the axis tracing out a pair of cones joined at their apices. The term "precession" typically refers only to this largest part of the motion; other changes in the alignment of Earth's axis—nutation and polar motion—are much smaller in magnitude. Earth's precession was historically called the precession of the equinoxes, because the equinoxes moved westward along the ecliptic relative to the fixed stars, opposite to the yearly motion of the Sun along the ecliptic.
Also note that the daily rotation of the Earth around its axis is opposite to the precessional rotation. When the polar axis precesses from one direction to another, then the equatorial plane of the Earth (indicated with the circular grid around the equator) and the associated celestial equator will move too. Where the celestial equator intersects the ecliptic (red line) there are the equinoxes. As seen from the drawing, the orange grid, 5000 years ago one intersection of equator and ecliptic, the vernal equinox was close to the star Aldebaran of Taurus.
The ecliptic coordinate system is a celestial coordinate system commonly used for representing the apparent positions and orbits of Solar System objects. Because most planets (except Mercury) and many small Solar System bodies have orbits with only slight inclinations to the ecliptic, using it as the fundamental plane is convenient. The system's origin can be the center of either the Sun or Earth, its primary direction is towards the vernal (March) equinox, and it has a right-hand convention. It may be implemented in spherical or rectangular coordinates.
A non-inclined orbit is an orbit coplanar with a plane of reference. The orbital inclination is 0° for prograde orbits, and π (180°) for retrograde ones. If the plane of reference is a massive spheroid body's equatorial plane, these orbits are called equatorial; if the plane of reference is the ecliptic plane, they are called ecliptic. As these orbits lack nodes, the ascending node is usually taken to lie in the reference direction (usually the vernal equinox), and thus the longitude of the ascending node is taken to be zero.
In the night sky over ESO's Very Large Telescope (VLT) observatory at Paranal, the Moon shines along with two bright companions: Venus and Jupiter. However, if two celestial bodies attain the same declination at the time of a conjunction in right ascension (or the same ecliptic latitude at a conjunction in ecliptic longitude), the one that is closer to the Earth will pass in front of the other. In such a case, a syzygy takes place. If one object moves into the shadow of another, the event is an eclipse.
The Earth in its orbit around the Sun causes the Sun to appear on the celestial sphere moving over the ecliptic (red), which is tilted on the equator (blue). The Zodiac is a group of 12 constellations: Leo, Virgo, Libra, Scorpius, Sagittarius, Capricornus, Aquarius, Pisces, Aries, Taurus, Gemini, and Cancer. Some version of these constellations are found in traditions around the world, for this band around the celestial sphere includes the ecliptic, the apparent path of the sun through the year. These constellations therefore are all associated with zodiac signs.
The globe itself has been manufactured in one piece, so as to be seamless. This complicated process was, if not invented, then certainly perfected, in the Lahore workshop Diya’ ad-din Muhammad worked in. There are grooves which encircle the surface of the globe that create 12 sections of 30° which pass through the ecliptic poles. While they are no longer used in astronomy today, they are called “ecliptic latitude circles” and help astronomers of the Arabic and Greek worlds find the co-ordinates of a particular star.
The nodes are points at which the Moon's orbit crosses the ecliptic. The Moon crosses the same node every 27.2122 days, an interval called the draconic month or draconitic month. The line of nodes, the intersection between the two respective planes, has a retrograde motion: for an observer on Earth, it rotates westward along the ecliptic with a period of 18.6 years or 19.3549° per year. When viewed from the celestial north, the nodes move clockwise around Earth, opposite to Earth's own spin and its revolution around the Sun.
A sidereal year (, ; from Latin "asterism, star") is the time taken by the Earth to orbit the Sun once with respect to the fixed stars. Hence, it is also the time taken for the Sun to return to the same position with respect to the fixed stars after apparently travelling once around the ecliptic. It equals for the J2000.0 epoch. The sidereal year differs from the tropical year, "the period of time required for the ecliptic longitude of the Sun to increase 360 degrees", due to the precession of the equinoxes.
Tycho's distinctive contributions to lunar theory include his discovery of the variation of the Moon's longitude. This represents the largest inequality of longitude after the equation of the center and the evection. He also discovered librations in the inclination of the plane of the lunar orbit, relative to the ecliptic (which is not a constant of about 5° as had been believed before him, but fluctuates through a range of over a quarter of a degree), and accompanying oscillations in the longitude of the lunar node. These represent perturbations in the Moon's ecliptic latitude.
This circle across the celestial sphere forms the apparent path of the Sun as the Earth completes its annual orbit. As the orbital plane of the Moon and the planets lie near the ecliptic, they can usually be found in the constellation Taurus during some part of each year. The galactic plane of the Milky Way intersects the northeast corner of the constellation and the galactic anticenter is located near the border between Taurus and Auriga. Taurus is the only constellation crossed by all three of the galactic equator, celestial equator, and ecliptic.
Wagner (2001), 75–76. Zhang provided a valuable description of his water-powered armillary sphere in the treatise of 125, stating: > The equatorial ring goes around the belly of the armillary sphere 91 and > 5/19 (degrees) away from the pole. The circle of the ecliptic also goes > round the belly of the instrument at an angle of 24 (degrees) with the > equator. Thus at the summer solstice the ecliptic is 67 (degrees) and a > fraction away from the pole, while at the winter solstice it is 115 > (degrees) and a fraction away.
The band has stated that the concept of Coma Ecliptic involves a man stuck in a coma, journeying through his past lives. It was added that the man faces a choice to either stay or move on to something better. Each song is its own episode in a fashion similar to "The Twilight Zone". Coma Ecliptic is notably the first album since 2005's Alaska to feature no songs over 10 minutes in length, and also the first album to have a smaller emphasis on growling compared to previous albums.
The orbit of Salacia is similar to Pluto, except for a near opposite longitude of ascending node. Its current position is near its most northern position above the ecliptic. Salacia is a non-resonant object with a moderate eccentricity (0.11) and large inclination (23.9°), making it a scattered–extended object in the classification of the Deep Ecliptic Survey and a hot classical in the classification system of Gladman et al., which may be a non-distinction if they are part of a single population that formed during the outward migration of Neptune.
In 2016, a modeled lightcurve using photometric data from various sources of an international collaboration of astronomers, rendered a concurring sidereal period of and two spin axes of (40.0°, 5.0°) and (225.0°, 16.0°) in ecliptic coordinates (λ, β).
Constellation boundaries are clearly but unobtrusively drawn. The celestial equator and ecliptic are indicated. The brightest radio sources are also shown. The Atlas Coeli is famous for its clean appearance and for the wealth of data it contains.
They gave a concurring sidereal period of 7.88695 and 7.88697 hours. Each of the studies also determined two spin axis in ecliptic coordinates (λ, β): (142.0°, −50.0°) and (305.0°, −45.0°), as well as (130.0°, −44.0°) and (312.0°, −51.0°).
In 2013 and 2016, an international study modeled a lightcurve with a concurring period of 31.0651 and 31.066 hours, respectively. The study also determined two spin axis of (299.0°, 42.0°) and (106.0°, 47.0°) in ecliptic coordinates (λ, β) ().
The asteroid orbits the Sun at a distance of 0.8–1.9 AU once every 1 years and 7 months (576 days). Its orbit has an eccentricity of 0.39 and an inclination of 14° with respect to the ecliptic.
This term is sometimes erroneously used for the draconic or nodal period of lunar precession, that is the period of a complete revolution of the Moon's ascending node around the ecliptic: Julian years ( days; at the epoch J2000.0).
For Earth-bound observers this occurs when the body in question is at opposition and on the ecliptic. The visual geometric albedo refers to the geometric albedo quantity when accounting for only electromagnetic radiation in the visible spectrum.
Hanuš et al. (2013) gives two possible solutions for the pole in ecliptic coordinates: (λ1, β1) = (287°, −39°) or (λ1, β1) = (102°, −55°). The estimated mass of 72 Feronia, and hence the density, has a large margin of error.
Guisan orbits the Sun in the central main-belt at a distance of 2.2–2.8 AU once every 4.02 years (1,467 days). Its orbit has an eccentricity of 0.12 and an inclination of 8° with respect to the ecliptic.
Its orbit has an eccentricity of 0.03 and an inclination of 24° with respect to the ecliptic. The body's observation arc begins at the discovering observatory (or at Simeiz Observatory), 15 days after its official discovery observation at Turku.
Its orbit has an eccentricity of 0.05 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with a precovery at Palomar in November 1954, almost 34 years prior to its official discovery observation.
Dworetsky orbits the Sun in the outer main-belt at a distance of 2.8–3.1 AU once every 5.03 years (1,839 days). Its orbit has an eccentricity of 0.04 and an inclination of 2° with respect to the ecliptic.
Its orbit has an eccentricity of 0.20 and an inclination of 13° with respect to the ecliptic. The first precovery was taken at Lowell Observatory in 1931, extending the asteroid's observation arc by 52 years prior to its discovery.
The asteroid's lightcurve has also been modeled using photometric data from the Lowell Photometric Database. It gave a concurring period of 5.65454 hours and determined two spin axis of (85.0°, −61.0°) and (271.0°, −31.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.15 and an inclination of 6° with respect to the ecliptic. In 1938, Oulu was first identified as at Bergedorf Observatory. Its observation arc, however, begins one month after its official discovery observation.
Prometheus orbits the Sun in the outer main-belt at a distance of 2.6–3.2 AU once every 5.00 years (1,827 days). Its orbit has an eccentricity of 0.10 and an inclination of 3° with respect to the ecliptic.
Its orbit has an eccentricity of 0.22 and an inclination of 1° with respect to the ecliptic. The first precovery was taken at Palomar Observatory in 1954, extending the asteroid's observation arc by 36 years prior to its discovery.
Based upon an annual parallax shift of 28.79 mas, the distance to this system is approximately . The system is located near the ecliptic, so it is subject to occultation by the Moon. The dynamical mass of the system is .
Lightcurve analysis indicates that Eugenia's pole most likely points towards ecliptic coordinates (β, λ) = (-30°, 124°) with a 10° uncertainty, which gives it an axial tilt of 117°. Eugenia's rotation is then retrograde, rotating backward to its orbital plane.
Using observations over 187 days Bessel computed an elongated orbit inclined about 63° to the ecliptic. At perihelion, which occurred on 19 September 1807 the comet was about .646 AU the Sun. The comet was on September 11 about .
In addition modeled lightcurves, using photometric data from the Lowell photometric database and other sources, gave a period of 9.37510 and 9.37514 hours, as well as a spin axis of (n.a., 65.0°) and (63.0°, 53.0°) in ecliptic coordinates, respectively ().
Lunisolar precession is caused by the gravitational forces of the Moon and Sun on Earth's equatorial bulge, causing Earth's axis to move with respect to inertial space. Planetary precession (an advance) is due to the small angle between the gravitational force of the other planets on Earth and its orbital plane (the ecliptic), causing the plane of the ecliptic to shift slightly relative to inertial space. Lunisolar precession is about 500 times greater than planetary precession. In addition to the Moon and Sun, the other planets also cause a small movement of Earth's axis in inertial space, making the contrast in the terms lunisolar versus planetary misleading, so in 2006 the International Astronomical Union recommended that the dominant component be renamed the precession of the equator, and the minor component be renamed precession of the ecliptic, but their combination is still named general precession.
Along with a later 17th-century Chinese illustration of Guo's mathematical proofs, Needham states that: > Guo used a quadrangular spherical pyramid, the basal quadrilateral of which > consisted of one equatorial and one ecliptic arc, together with two meridian > arcs, one of which passed through the summer solstice point...By such > methods he was able to obtain the du lü (degrees of equator corresponding to > degrees of ecliptic), the ji cha (values of chords for given ecliptic arcs), > and the cha lü (difference between chords of arcs differing by 1 > degree).Needham, Volume 3, 109–110. Despite the achievements of Shen and Guo's work in trigonometry, another substantial work in Chinese trigonometry would not be published again until 1607, with the dual publication of Euclid's Elements by Chinese official and astronomer Xu Guangqi (1562-1633) and the Italian Jesuit Matteo Ricci (1552-1610).Needham, Volume 3, 110.
The orbital plane is inclined by an angle of 5.4° to the plane of the ecliptic. This is a spectral type TDG asteroid with a cross-section size of 84 km. The asteroid has an estimated rotation period of 8.09 h.
In 2013, the asteroid's lightcurve was also modeled from combined dense and sparse photometry. It gave a concurring sidereal period of 4.714793 hours. The modelling also determined two spin axis of (345.0°, −22.0°) and (173.0°, −3.0°) in ecliptic coordinates (λ, β).
In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue and other sources gave a concurring sidereal period of 3.081545 hours, as well as two spin axis of (268.0°, 23.0°) and (87.0°, 28.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.11 and an inclination of 11° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar in August 1988, just two months prior to its official discovery observation.
Its orbit has an eccentricity of 0.12 and an inclination of 11° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar in July 1951, more than 37 years prior to its official discovery observation.
Its orbit has an eccentricity of 0.11 and an inclination of 25° with respect to the ecliptic. The body's observation arc begins with its first observation at Palomar in September 1988, just one month prior to its official discovery observation.
Its orbit has an eccentricity of 0.21 and an inclination of 34° with respect to the ecliptic. The body's observation arc begins at the Yerkes Observatory in April 1933, or two months after its official discovery observation at Oak Ridge.
Its orbit has an eccentricity of 0.02 and an inclination of 27° with respect to the ecliptic. The body's observation arc begins with its first observation as ' at Palomar in September 1988, or one year prior to its official discovery observation.
Its orbit has an eccentricity of 0.05 and an inclination of 25° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar in March 1956, or 33 years prior to its official discovery observation.
Its orbit has an eccentricity of 0.06 and an inclination of 24° with respect to the ecliptic. The body's observation arc begins with a precovery at Palomar in July 1950, more than 38 years prior to its official discovery observation.
Its orbit has an eccentricity of 0.04 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins with its first observation at Palomar in August 1988, just one month prior to its official discovery observation.
In 2016, a rotational lightcurve of Riceia was modeled from photometric data from the Lowell Photometric Database. Lightcurve analysis gave a sidereal rotation period of 6.67317 hours as well as a spin axis of (37.0°, −63.0°) in ecliptic coordinates (λ, β).
Between 2011 and 2017, an international collaboration modeled three lightcurves with a period of 5.794995, 5.79500 and 5.79501 hours, respectively. The more recent studies also determined two spin axis of (155.0°, 25.0°) and (331.0°, 5.0°) in ecliptic coordinates (λ, β).
The asteroid's lightcurve has also been modeled several times. It gave a concurring period of 44.6768 and 44.677 hours, respectively. Modelling in the 2018-study also gave two spin axis of (127.0°, −43.0.0°) and (280.0°, −44.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.05 and an inclination of 22° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar in December 1950, more than 37 years prior to its official discovery observation.
Its orbit has an eccentricity of 0.13 and an inclination of 3° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar in April 1954, or 29 years prior to its official discovery observation.
The asteroid's lightcurve has also been modeled several times and gave a concurring period of 6.54448 and 6.54449 hours, respectively. The body's spin axis has also been determined to be at (146.0°, −2.0°) and (326.0°, −2.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.20 and an inclination of 7° with respect to the ecliptic. The asteroid's observation arc begins 42 years prior to its official discovery observation, with a precovery taken at the Palomar Observatory in September 1960.
IC 1517 is an elliptical galaxy, of apparent magnitude +13.8, in the constellation Pisces. The galaxy is south and west of Gamma Piscium, just south of the ecliptic, and north of the constellation Aquarius. It has a redshift of 0.02449.
The starting point for this is always the first point of spring (the vernal equinox) or 0º0' Aries, ending at 29º59' Pisces. This is the tropical zodiac, a ‘belt’ of sky extending about 8–9 degrees either side of the ecliptic.
Mean longitude is the ecliptic longitude at which an orbiting body could be found if its orbit were circular and free of perturbations. While nominally a simple longitude, in practice the mean longitude does not correspond to any one physical angle.
Its orbit has an eccentricity of 0.08 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar in September 1953, or 25 years prior to its official discovery observation.
Its orbit has an eccentricity of 0.05 and an inclination of 5° with respect to the ecliptic. The first precovery was taken at the U.S. Palomar Observatory in 1953, extending the asteroid's observation arc by 44 years prior to it discovery.
In 2016, the asteroid's lightcurve has been modeled using data from Lowell photometric database, which gave a sidereal rotation period of 7.43019 hours, as well as two spin axes of (72.0°, −64.0°) and (288.0°, −55.0°) in ecliptic coordinates (λ, β) ().
By August 15, 2013, it was decided that the wheels were unrecoverable, and an engineering report was ordered to assess the spacecraft's remaining capabilities. This effort ultimately led to the "K2" follow-on mission observing different fields near the ecliptic.
Because the Earth's equator is itself inclined at an angle of about 23.4° to the ecliptic (the obliquity of the ecliptic, \epsilon), these effects combine to vary the inclination of the Moon's orbit to the equator by between 18.4° and 28.6° over the 18.6 year period. This causes the orientation of the Earth's axis to vary over the same period, with the true position of the celestial poles describing a small ellipse around their mean position. The maximum radius of this ellipse is the constant of nutation, approximately 9.2 arcseconds. Smaller effects also contribute to nutation.
Tempel 1, a Jupiter-family comet The Kuiper belt was initially thought to be the source of the Solar System's ecliptic comets. However, studies of the region since 1992 have shown that the orbits within the Kuiper belt are relatively stable, and that ecliptic comets originate from the scattered disc, where orbits are generally less stable. Comets can loosely be divided into two categories: short-period and long-period—the latter being thought to originate in the Oort cloud. The two major categories of short- period comets are Jupiter-family comets (JFCs) and Halley-type comets.
The twelve signs of the zodiac, miniatures from a book of hours. (The Sky: Order and Chaos by Jean-Pierre Verdet, from the 'New Horizons' series) In Western astrology, astrological signs are the twelve 30° sectors of the ecliptic, starting at the vernal equinox (one of the intersections of the ecliptic with the celestial equator), also known as the First Point of Aries. The order of the astrological signs is Aries, Taurus, Gemini, Cancer, Leo, Virgo, Libra, Scorpio, Sagittarius, Capricorn, Aquarius and Pisces. Each sector was named for a constellation within it in the time of naming.
Cetus is not among the 12 true zodiac constellations in the J2000 epoch, nor classical 12-part zodiac. The ecliptic passes less than 0.25° from one of its corners. Thus the moon and planets will enter Cetus (occulting any stars as a foreground object) in 50% of their successive orbits briefly and the southern part of the sun appears in Cetus for about one day each year. Many asteroids in belts have longer phases occulting the north-western part of Cetus, that bulk with a slightly greater inclination to the ecliptic than the moon and planets.
A quasi- satellite, such as the one shown in this diagram, moves in a prograde orbit around the Sun, with the same orbital period (which we will call a year) as the planet it accompanies, but with a different (usually greater) orbital eccentricity. It appears, when seen from the planet, to revolve around the planet once a year in the retrograde direction, but at varying speed and probably not in the ecliptic plane. Relative to its mean position, moving at constant speed in the ecliptic, the quasi-satellite traces an analemma in the planet's sky, going around it once a year.
The moon's orbit is not in the same plane as the Earth's orbit around the sun but crosses it in two places. The moon crosses the ecliptic plane twice a month, once when it goes up above the plane, and again 15 or so days later when it goes back down below the ecliptic. These two locations are the ascending and descending lunar nodes. Solar and lunar eclipses will occur only when the moon is positioned near one of these nodes because at other times the moon is either too high or too low for an eclipse to be noticed from the earth.
On the front face of the mechanism there is a fixed ring dial representing the ecliptic, the twelve zodiacal signs marked off with equal 30-degree sectors. This matched with the Babylonian custom of assigning one twelfth of the ecliptic to each zodiac sign equally, even though the constellation boundaries were variable. Outside that dial is another ring which is rotatable, marked off with the months and days of the Sothic Egyptian calendar, twelve months of 30 days plus five intercalary days. The months are marked with the Egyptian names for the months transcribed into the Greek alphabet.
However, is not a plutino, as it is not actually in a resonance with Neptune, and it may have formed near its present nearly circular orbit lying almost perfectly on the ecliptic. This TNO may have remained dynamically cold since its formation, and thus its orbit may not have been a direct result of significant perturbations from Neptune during its migration to the outer solar system. The Deep Ecliptic Survey (DES) currently classifies it as a cubewano (classical) based on a 10-million-year integration of the orbit. File:2002KX14-orbit.png comes to opposition in late May at an apparent magnitude of 20.4.
The large dial in the middle of the front has a fixed Zodiac and two hands showing the position of the Sun and the Moon on the ecliptic circle. The Sun hand makes one revolution every year, and the Moon hand one revolution every 29.5 day. This dial also shows when and where solar and lunar eclipses occur. The orbit of the Moon has an inclination of 5° with regard to the ecliptic, so solar or lunar eclipses can only occur when the Sun and the Moon are simultaneously located at one of the crossings of the two orbits.
The orbit is inclined by 18° to the ecliptic, with much of it lying south of the ecliptic. (Because it is retrograde, the true inclination is 162°.) Owing to the retrograde orbit, it has one of the highest velocities relative to the Earth of any object in the Solar System. The 1910 passage was at a relative velocity of 70.56 km/s (157,838 mph or 254,016 km/h). Because its orbit comes close to Earth's in two places, Halley is associated with two meteor showers: the Eta Aquariids in early May, and the Orionids in late October.
The orbit of Eris (blue) compared to those of Saturn, Uranus, Neptune, and Pluto (white/gray). The arcs below the ecliptic are plotted in darker colors, and the red dot is the Sun. The diagram on the left is a polar view whereas the diagrams on the right are different views from the ecliptic. Eris has an orbital period of 559 years. Its maximum possible distance from the Sun (aphelion) is 97.65 AU, and its closest (perihelion) is 37.91 AU. It came to perihelion between 1698 and 1699, and to aphelion around 1977, and will return to perihelion around 2256 to 2258.
The reference frame is relatively stationary, aligned with the vernal equinox. A rectangular variant of ecliptic coordinates is often used in orbital calculations and simulations. It has its origin at the center of the Sun (or at the barycenter of the Solar System), its fundamental plane on the ecliptic plane, and the -axis toward the vernal equinox. The coordinates have a right-handed convention, that is, if one extends their right thumb upward, it simulates the -axis, their extended index finger the -axis, and the curl of the other fingers points generally in the direction of the -axis.
The rotation period of Siarnaq was measured by the Cassini spacecraft to be 10.19 hours; this is the shortest rotation period of all prograde irregular moons of Saturn. Siarnaq displays a light curve with three maxima and minima over a full rotation, implying a roughly triangular shape. From Cassini observations of Siarnaq at different phase angles, the orientation of its north rotational pole has been determined to be pointing toward 98° ecliptic latitude and −23° ecliptic longitude. This corresponds to a sideways axial tilt, indicating that Siarnaq experiences long, extreme seasons similar to the planet Uranus.
Zodiac chart with dodecatemoria shown within the sign of Aries Dodecatemoria are subdivisions of the twelve signs of the Zodiac into a further twelve parts each. These can be said to form a "micro-zodiac" of 144 dodecatemoria, each corresponding to 2.5° of the ecliptic. In an alternate usage, the dodecamorion refers to a point on the ecliptic reached by the addition of twelve times a given number of degrees within a sign, either to the original degree, or to the beginning of the sign. This system, used in Hellenistic astrology but less favored by later ages, apparently originated in Babylonian astrology.
Ulysses sits atop the PAM-S and IUS combination Illustration of Ulysses after deployment Illustration of Solar Polar on IUS Until Ulysses, the Sun was only observed from low solar latitudes. The Earth's orbit defines the ecliptic plane, which differs from the Sun's equatorial plane by only 7.25 degrees. Even spacecraft directly orbiting the Sun do so in planes close to the ecliptic because a direct launch into a high-inclination solar orbit would require a prohibitively large launch vehicle. Several spacecraft (Mariner 10, Pioneer 11, and Voyagers 1 and 2) had performed gravity assist manoeuvres in the 1970s.
Ancient Chinese astronomers divided the sky ecliptic into four regions, collectively known as the Four Symbols, each assigned a mysterious animal. They are Azure Dragon (青龍) on the east, Black Tortoise (玄武) on the north, White Tiger (白虎) on the west, and Vermilion Bird (朱雀) on the south. Each region contains seven mansions, making a total of 28 mansions. These mansions or xiù correspond to the longitudes along the ecliptic that the Moon crosses during its 27.32-day journey around the Earth and serve as a way to track the Moon's progress.
The sidereal year of 365.25636 days is only valid for stars on the ecliptic (the apparent path of the Sun across the sky), whereas Sirius's displacement ~40° below the ecliptic, its proper motion, and the wobbling of the celestial equator cause the period between its heliacal risings to be almost exactly 365.25 days long instead. This steady loss of one relative day every four years over the course of the 365-day calendar meant that the "wandering" day would return to its original place relative to the solar and Sothic year after precisely 1461 civil or 1460 Julian years.
In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from a large collaboration of individual observers (such as above). The study also determined two spin axes of (42.0°, 44.0°) and (226.0°, 73.0°) in ecliptic coordinates (λ, β).
In 2018, Czech astronomers Josef Ďurech and Josef Hanuš published a modeled lightcurve using photometric data from the Gaia spacecraft's second data release. It showed a sidereal period of hours (), and gave a spin axis at (18.0°, 78.0°) in ecliptic coordinates (λ, β).
Encyclopedia of the Solar System. San Diego: Academic Press. Page 218. As of 2011, over 200 SDOs have been identified, including Gǃkúnǁʼhòmdímà (discovered by Schwamb, Brown, and Rabinowitz), (NEAT), Eris (Brown, Trujillo, and Rabinowitz), Sedna (Brown, Trujillo, and Rabinowitz) and (Deep Ecliptic Survey).
Ibarruri orbits the Sun in the inner main-belt at a distance of 1.6–2.8 AU once every 3 years and 3 months (1,183 days). Its orbit has an eccentricity of 0.28 and an inclination of 4° with respect to the ecliptic.
Its orbit has an eccentricity of 0.13 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar Observatory in December 1951, nearly three decades prior to its official discovery observation La Silla.
Cuyo orbits the Sun at a distance of 1.1–3.2 AU once every 3 years and 2 months (1,151 days; semi-major axis of 2.15 AU). Its orbit has an eccentricity of 0.51 and an inclination of 24° with respect to the ecliptic.
Efimov orbits the Sun in the inner main-belt at a distance of 1.7–2.7 AU once every 3 years and 4 months (1,214 days). Its orbit has an eccentricity of 0.23 and an inclination of 6° with respect to the ecliptic.
The asteroid orbits the Sun in the inner main-belt at a distance of 1.6–2.9 AU once every 3 years and 5 months (1,260 days). Its orbit has an eccentricity of 0.28 and an inclination of 4° with respect to the ecliptic.
Ahti orbits the Sun in the outer main-belt at a distance of 3.1–3.4 AU once every 5 years and 9 months (2,115 days). Its orbit has an eccentricity of 0.05 and an inclination of 15° with respect to the ecliptic.
Bengt orbits the Sun in the inner main-belt at a distance of 2.0–2.7 AU once every 3 years and 7 months (1,306 days). Its orbit has an eccentricity of 0.14 and an inclination of 3° with respect to the ecliptic.
Its orbit has an eccentricity of 0.13 and an inclination of 22° with respect to the ecliptic. In 1973, it was first identified as at Lick Observatory, extending the body's observation arc by 17 years prior to its official discovery observation at Palomar.
The asteroids lightcurve has also been modeled, using photometric data from the Lowell Photometric Database and other sources. Modelling gave a concurring period of 12.18978 hours, as well as two spin axis of (19.0°, 44°) and (250.0°, 64°) in ecliptic coordinates (λ, β).
The asteroid orbits the Sun in the inner main-belt at a distance of 2.1–2.4 AU once every 3 years and 4 months (1,231 days). Its orbit has an eccentricity of 0.08 and an inclination of 3° with respect to the ecliptic.
Its orbit has an eccentricity of 0.11 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins with its first observation as at Kiso Observatory in November 1982, more than 15 years prior to its official discovery observation.
Lyyli orbits the Sun in the central main-belt at a distance of 1.5–3.6 AU once every 4 years and 2 months (1,522 days). Its orbit has an eccentricity of 0.41 and an inclination of 21° with respect to the ecliptic.
Its orbit has an eccentricity of 0.10 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Heidelberg Observatory in October 1915, or 62 years prior to its official discovery observation at Zimmerwald.
Its orbit has an eccentricity of 0.13 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins with its first observation as at Heidelberg in November 1907, more than 16 years prior to its official discovery observation.
' orbits the Sun at a distance of 1.0–2.7 AU once every 2 years and 7 months (932 days; semi-major axis of 1.87 AU). Its orbit has an eccentricity of 0.45 and an inclination of 1° with respect to the ecliptic.
The WAVES and MFI experiments were designed to measure the electric and magnetic fields observed in the solar wind. All together, the Wind spacecraft's suite of instruments allows for a complete description of plasma phenomena in the solar wind plane of the ecliptic.
Tombaugh was given the job of hunting for a suspected "9th planet" to be achieved by systematically photographing the area of the sky around the ecliptic. Tombaugh used Lowell Observatory's (3 lens element), f/5.3 refractor astrograph, which recorded images on glass plates.
The asteroid orbits the Sun in the outer main-belt at a distance of 2.7–3.5 AU once every 5 years and 5 months (1,992 days). Its orbit has an eccentricity of 0.13 and an inclination of 4° with respect to the ecliptic.
Its orbit has an eccentricity of 0.17 and an inclination of 23° with respect to the ecliptic. The body's observation arc begins with a precovery taken at the Palomar Observatory in June 1950, more than 40 years prior to its official discovery observation.
This so-called planetary precession shift amounts to a rotation of the ecliptic plane of 0.47 seconds of arc per year (more than a hundred times smaller than lunisolar precession). The sum of the two precessions is known as the general precession.
Its orbit has an eccentricity of 0.08 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins with a precovery at Palomar Observatory in March 1953, almost 24 years prior to its official discovery observation at Kiso.
For the orbit of the Moon around Earth, the plane is taken to be the ecliptic, not the equatorial plane. The gravitational pull of the Sun upon the Moon causes its nodes to gradually precess westward, completing a cycle in approximately 18.6 years.
Wesson orbits the Sun in the inner main belt at a distance of 1.8–2.7 AU, orbiting once every 3 years and 5 months (1,235 days). Its orbit has an eccentricity of 0.19 and an inclination of 5° with respect to the ecliptic.
Spicer orbits the Sun in the central main-belt at a distance of 2.1–3.3 AU once every 4 years and 5 months (1,619 days). Its orbit has an eccentricity of 0.23 and an inclination of 6° with respect to the ecliptic.
It is classified as a detached object by the Deep Ecliptic Survey (DES), since its orbit appears to be beyond the current control of Neptune. Though, if Neptune migrated outward, there would have been a period when Neptune had a higher eccentricity.
Its orbit has an eccentricity of 0.05 and an inclination of 5° with respect to the ecliptic. In 1931, Beograd was first identified as at Uccle Observatory, extending the body's observation arc by 7 years prior to its official discovery observation at Belgrade.
Ingeborg orbits the Sun in the inner main-belt at a distance of 1.6–3.0 AU once every 3 years and 6 months (1,291 days). Its orbit has an eccentricity of 0.31 and an inclination of 23° with respect to the ecliptic.
Atlas , designation 27 Tauri, is a triple star system in the constellation of Taurus. It is a member of the Pleiades, an open star cluster (M45). It is 431 light-years (132 parsecs) away, and is 3.92 degrees north of the ecliptic.
It orbits the Sun at a distance of 0.6–3.5 AU once every 2 years and 11 months (1,073 days; semi-major axis of 2.05 AU). Its orbit has an eccentricity of 0.71 and an inclination of 6° with respect to the ecliptic.
Its orbit has an eccentricity of 0.15 and an inclination of 16° with respect to the ecliptic. The body's observation arc begins at Vienna Observatory on 8 May 2013, or two weeks after its official discovery observation by Grigory Neujmin at Simeiz.
Its orbit has an eccentricity of 0.19 and an inclination of 1° with respect to the ecliptic. The body's observation arc begins with a precovery taken by Spacewatch in November 1996, or 14 months prior to its official discovery observation at Socorro.
It orbits the Sun at a distance of 38.1–592.0 AU once every 5591 years and 11 months (2,042,441 days; semi-major axis of 315.04 AU). Its orbit has an eccentricity of 0.88 and an inclination of 7° with respect to the ecliptic.
Its orbit has an eccentricity of 0.06 and an inclination of 25° with respect to the ecliptic. It has the same orbital period as Neptune and orbits at the Lagrangian point about 60° ahead of Neptune. It has an inclination of 25 degrees.
Its orbit has an eccentricity of 0.02 and an inclination of 17° with respect to the ecliptic. The body's observation arc begins with its first observation as ' at Palomar Observatory in January 1982, more than 16 years prior to its official discovery observation at Socorro.
Its orbit has an eccentricity of 0.04 and a high inclination of 43° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar Observatory in September 1953, or 46 years prior to its official discovery observation at Fountain Hills.
Its orbit has an eccentricity of 0.16 and an inclination of 14° with respect to the ecliptic. The body's observation arc begins with its first identification as ' at Heidelberg Observatory in October 1908, more than 13 years prior to its official discovery observation at Nice.
Its orbit has an eccentricity of 0.22 and an inclination of 2° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar Observatory in February 1977, or four years prior to its official discovery observation at Siding Spring.
Its orbit has an eccentricity of 0.05 and an inclination of 17° with respect to the ecliptic. The body's observation arc begins with its first observation as ' at El Leoncito in April 1967, nearly 33 years prior to its official discovery observation at Socorro.
The Minor Planet Center (MPC) classifies it as a cubewano. But since this object has an inclination of 19.3°, the Deep Ecliptic Survey (DES) classifies it as scattered-extended. It has been observed 119 times over thirteen oppositions, with precovery images back to 1954.
Its orbit has an eccentricity of 0.12 and an inclination of 3° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Crimea–Nauchnij in September 1985, just three weeks prior to its official discovery observation at Anderson Mesa.
Its orbit has an eccentricity of 0.15 and an inclination of 15° with respect to the ecliptic. The asteroid was first observed as ' at Crimea–Nauchnij in July 1973. The body's observation arc begins with its official discovery observation at Caussols in January 1993.
The C-type asteroid orbits the Sun in the middle main-belt at a distance of 2.3–3.2 AU once every 4 years and 6 months (1,653 days). Its orbit has an eccentricity of 0.18 and an inclination of 12° with respect to the ecliptic.
Its orbit has an eccentricity of 0.09 and an inclination of 24° with respect to the ecliptic. The body's observation arc begins with a precovery taken at the Palomar Observatory in November 1954, nearly 36 years prior to its official discovery observation at Tautenburg.
The S-type asteroid orbits the Sun in the central main-belt at a distance of 2.2–3.1 AU once every 4 years and 3 months (1,546 days). Its orbit has an eccentricity of 0.17 and an inclination of 14° with respect to the ecliptic.
Its orbit has an eccentricity of 0.07 and an inclination of 16° with respect to the ecliptic. The body's observation arc begins with a precovery taken at the Siding Spring Observatory in March 1980, almost 8 years prior to its official discovery observation at Palomar.
Its orbit has an eccentricity of 0.05 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar Observatory in December 1951, more than 36 years prior to its official discovery observation at La Silla.
Its orbit has an eccentricity of 0.04 and an inclination of 10° with respect to the ecliptic. The body's observation arc begins with its first observation at the La Silla Observatory in February 1990, or 14 months prior to its official discovery observation at Palomar.
Its orbit has an eccentricity of 0.06 and an inclination of 8° with respect to the ecliptic. Brauna was first identified as at Simeiz Observatory in September 1929. The body's observation arc begins at the discovering Heidelberg Observatory, one month after its official discovery observation.
Its orbit has an eccentricity of 0.20 and an inclination of 12° with respect to the ecliptic. The asteroid was first observed as at Simeiz Observatory in October 1917. The body's observation arc begins with its official discovery observation at Algiers in March 1936.
A one-hour video recording of the event was featured on the LDS Church home page. Lindsey has a celestial body named after her, Asteroid 242516 Lindseystirling, about 2–3 km diameter, semi-major axis of 2.72AU, eccentricity of 0.051, inclined 3.7 degrees to ecliptic.
Its orbit has an eccentricity of 0.09 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins with its first observations as at Crimea–Nauchnij in April 1970, about 16 years prior to its official discovery observation at Brorfelde.
The C-type minor planet orbits the Sun at a distance of 34–65 AU once every 346 years (126,383 days; semi-major axis of 49.29 AU). Its orbit has an eccentricity of 0.31 and an inclination of 25° with respect to the ecliptic.
Its orbit has an eccentricity of 0.05 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins with its first observation as ' at La Silla in April 1992, or four and a half years prior to its official discovery observation.
Its orbit has an eccentricity of 0.02 and an inclination of 6° with respect to the ecliptic. Menelaus was first imaged at Palomar in November 1951. This precovery extends the body's observation arc by more than 5 years prior to its official discovery observation.
In 2016, a rotational lightcurve of Carelia was published using modeled photometric data from the Lowell Photometric Database (LPD). Lightcurve analysis gave a rotation period of hours (), as well as two spin axes at (21.0°, −79.0°) and (208.0°, −43.0°) in ecliptic coordinates (λ, β).
The dark asteroid orbits the Sun in the outer main-belt at a distance of 2.7–3.5 AU once every 5 years and 7 months (2,035 days). Its orbit has an eccentricity of 0.13 and an inclination of 13° with respect to the ecliptic.
Its orbit has an eccentricity of 0.22 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins with its first observation as at Turku Observatory in April 1940, or 32 years prior to its official discovery observation at Nauchnyj.
Based on his many photometric observations, astronomer Maurice Clark also modeled the shape of Sheragul and obtained two spin axis with (306.0°, −35.8°) and (117.3°, −28.9°) in ecliptic coordinates (λ, β), respectively (). His observations also suggest that the asteroid is in a retrograde rotation.
Its orbit has an eccentricity of 0.15 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins with its first observation as ' at Heidelberg Observatory in September 1949, or 36 years prior to its official discovery observation at Palomar.
A conjunction is an apparent phenomenon caused by the observer's perspective: the two objects involved are not actually close to one another in space. Conjunctions between two bright objects close to the ecliptic, such as two bright planets, can be seen with the naked eye.
The S-type asteroid orbits the Sun in the inner main-belt at a distance of 1.9–3.0 AU once every 3 years and 9 months (1,377 days). Its orbit has an eccentricity of 0.23 and an inclination of 2° with respect to the ecliptic.
Its orbit has an eccentricity of 0.14 and an inclination of 19° with respect to the ecliptic. The body's observation arc begins with its first observation as ' at Palomar Observatory in September 1989, just two months prior to its official discovery observation at La Silla.
The S-type asteroid orbits the Sun in the inner main-belt at a distance of 1.5–2.9 AU once every 3 years and 3 months (1,174 days). Its orbit has an eccentricity of 0.33 and an inclination of 6° with respect to the ecliptic.
Its orbit has an eccentricity of 0.02 and an inclination of 28° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar Observatory in April 1954, more than 31 years prior to its official discovery observation at Kitt Peak.
Its orbit has an eccentricity of 0.09 and an inclination of 16° with respect to the ecliptic. A first precovery was taken at Palomar Observatory in September 1953, extending the body's observation arc by 35 years prior to its official discovery observation at Brorfelde.
The gravitational tidal forces of the Moon and Sun apply torque to the equator, attempting to pull the equatorial bulge into the plane of the ecliptic, but instead causing it to precess. The torque exerted by the planets, particularly Jupiter, also plays a role.
Both components are eclipsed (occulted) by the sun from about 7–9 November.In the Sky Earth astronomy reference utility showing the ecliptic and relevant date as at J2000 - present Thus the star can be viewed the whole night, crossing the sky, in early May.
Themisto was later lost (i.e. its orbit was not known well enough to reobserve it) and was not rediscovered until 2000. Between December 1976 and February 1985, Kowal searched 6400 square degrees of sky in the ecliptic plane for distant, slow-moving Solar System objects.
Its orbit has an eccentricity of 0.13 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar Observatory in June 1954, more than 31 years prior to its official discovery observation at Anderson Mesa.
Radar observation during 2001 encounter orbits the Sun at a distance of 0.42–1.02 AU once every 7 months (222 days; semi-major axis of 0.72 AU). Its orbit has an eccentricity of 0.42 and an inclination of 7° with respect to the ecliptic.
Its orbit has an eccentricity of 0.04 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with a precovery taken at the Palomar Observatory in August 1988, more than 5 years prior to its official discovery observation at Kushiro.
2020 JJ orbits the Sun at a distance of 0.9–2.1 AU once every 1 years and 10 months (675 days; semi-major axis of 1.51 AU). Its orbit has an eccentricity of 0.42 and an inclination of 11° with respect to the ecliptic.
It gave a period of 2.978 hours and an amplitude of 0.25 magnitude (). In 2016, an international study modeled a lightcurve with a concurring period of 2.978301 hours and found a spin axis of (277.0°, 57.0°) and (66.0°, 48.0°) in ecliptic coordinates (λ, β) ().
Its orbit has an eccentricity of 0.08 and an inclination of 21° with respect to the ecliptic. The body's observation arc begins with its observation as at Goethe Link Observatory in October 1963, more than 35 years after its official discovery observation at Heidelberg.
Animation of Pluto orbit from 1900 to 2100 Pluto's orbital period is currently about 248 years. Its orbital characteristics are substantially different from those of the planets, which follow nearly circular orbits around the Sun close to a flat reference plane called the ecliptic. In contrast, Pluto's orbit is moderately inclined relative to the ecliptic (over 17°) and moderately eccentric (elliptical). This eccentricity means a small region of Pluto's orbit lies closer to the Sun than Neptune's. The Pluto–Charon barycenter came to perihelion on September 5, 1989, and was last closer to the Sun than Neptune between February 7, 1979, and February 11, 1999.
Tombaugh continued searching for over a decade after the discovery of Pluto, and the lack of further discoveries left him satisfied that no other object of a comparable apparent magnitude existed near the ecliptic. No more trans-Neptunian objects were discovered until 15760 Albion in 1992. However, more recently the relatively bright object has been discovered. It has a relatively high orbital inclination, but at the time of Tombaugh's discovery of Pluto, Makemake was only a few degrees from the ecliptic near the border of Taurus and Aurigabased on Minor Planet Center online Minor Planet Ephemeris Service: March 1, 1930: RA: 05h51m, Dec: +29.0 at an apparent magnitude of 16.
Clyde Tombaugh, discoverer of Pluto The long road from planethood to reconsideration undergone by Ceres is mirrored in the story of Pluto, which was named a planet soon after its discovery by Clyde Tombaugh in 1930. Uranus and Neptune had been declared planets based on their circular orbits, large masses and proximity to the ecliptic plane. None of these applied to Pluto, a tiny and icy world in a region of gas giants with an orbit that carried it high above the ecliptic and even inside that of Neptune. In 1978, astronomers discovered Pluto's largest moon, Charon, which allowed them to determine its mass.
This is characteristic of all plutinos, which have orbital periods around 250 years and semi-major axes around 39 AU. Like Pluto, Ixion's orbit is elongated and inclined to the ecliptic. Ixion has an orbital eccentricity of 0.24 and an orbital inclination of 19.6 degrees, slightly greater than Pluto's inclination of 17 degrees. Over the course of its orbit, Ixion's distance from the Sun varies from 30.1 AU at perihelion (closest distance) to 39.8 AU at aphelion (farthest distance). Although Ixion's orbit is similar to that of Pluto, their orbits are oriented differently: Ixion's perihelion is below the ecliptic whereas Pluto's is above it (see right image).
The draconic year, draconitic year, eclipse year, or ecliptic year is the time taken for the Sun (as seen from the Earth) to complete one revolution with respect to the same lunar node (a point where the Moon's orbit intersects the ecliptic). The year is associated with eclipses: these occur only when both the Sun and the Moon are near these nodes; so eclipses occur within about a month of every half eclipse year. Hence there are two eclipse seasons every eclipse year. The average duration of the eclipse year is : days (346 d 14 h 52 min 54 s) (at the epoch J2000.0).
The estimated age is 1.6 billion years. It has an apparent visual magnitude of +3.53, allowing it to be seen with the naked eye. It is 0.18 degree south of the ecliptic so it is occasionally occulted by the Moon and, rarely, by a planet; and is eclipsed by the sun from about 10-12 July.In the Sky Earth astronomy reference utility showing the ecliptic and relevant date as at J2000 - present Thus the star can be viewed the whole night, crossing the sky, in mid-January. The last occultation by a planet was by Saturn on June 30, 1857, and the next will be by Venus on August 12, 2420.
The tidal locking of the planet may have occurred hundreds of millions of years ago, and seasons appear to be limited to the slight wobbling of the planet on the ecliptic. Far from being an uninteresting planet, the ecliptic along which the planet travels is also tilted. Most of the colonies are located along the "coast" - the place in a murky half-shadow of constant night and constant day. Scientific researchers from all kinds of alien species from all over the known universe have come to this planet to engage in an arduous archaeological expedition to unearth mysterious fossils from deep within the multi-kilometer thick icy crust.
Its orbit has an eccentricity of 0.04 and an inclination of 27° with respect to the ecliptic. The body's observation arc begins with its first observation as ' at the Goethe Link Observatory in November 1945, almost 56 years prior to its official discovery observation at Socorro.
In 2018, Czech astronomers Josef Ďurech and Josef Hanuš published a modeled lightcurve using photometric data from the Gaia probe's second data release. It showed a sidereal period of hours (), and gave two spin axes at (37.0°, 24.0°) and (220.0°, 7.0°) in ecliptic coordinates (λ, β).
Narvi is about 7 kilometres in diameter, and orbits Saturn at an average distance of 19,371,000 km in 1006.541 days, at an inclination of 137° to the ecliptic (109° to Saturn's equator), in a retrograde direction and with an eccentricity of 0.320. Narvi's rotation period is hours.
Modeled photometric data from the Lowell Photometric Database (LPD) and the robotic BlueEye600 Observatory, gave a concurring period of 19.9020 hours, Both studies determined two spin axes of (124.0°, −70.0°) and (266.0°, −62.0°), as well as (271.0°, −53.0°) and (115.0°, −62.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.07 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with its first observation as ' at Goethe Link Observatory in September 1955, more than 35 years prior to its official discovery observation at Toyota.
Kukarkin orbits the Sun in the outer main-belt at a distance of 2.0–3.9 AU once every 5.03 years (1,838 days). Its orbit has an eccentricity of 0.31 and an inclination of 15° with respect to the ecliptic. No precoveries were taken prior to its discovery.
Its orbit has an eccentricity of 0.52 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins with a precovery taken at the Siding Spring Observatory on in July 1981, more than 18 years prior to its official discovery observation at Haleakala.
Photometric data gathered with the 60-centimeter BlueEye600 robotic observatory near the Ondřejov Observatory in the Czech Republic, were used to model a lightcurve with a concurring period of 2.787153 hours and two spin axis of (142.0°, 40.0°) and (349.0°, 56.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.05 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with a precovery taken by Spacewatch at Kitt Peak Observatory in December 1995, more than 6 years prior to its official discovery observation at Palomar.
The ecliptic passes through the twelve constellations of the zodiac in the course of a year. Sundial in Singapore Botanic Gardens. The fact that Singapore is located almost at the equator is reflected in its design. This model of the Sun's motion helps to understand sundials.
Its orbit has an eccentricity of 0.12 and an inclination of 21° with respect to the ecliptic. The body's observation arc begins with its first observation as ' at the Kiso Observatory in November 1986, or 13 months prior to its official discovery observation at La Silla.
Its orbit has an eccentricity of 0.15 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins with its first observations as at Crimea-Nauchnij in October 1980, more than 15 years prior to its official discovery observation at Cima Ekar.
The asteroids lightcurve has also been modeled, using photometric data from the Lowell Photometric Database (LPD) and other sources. Modelling gave a concurring period of 43.179 and 43.1795 hours, as well as two spin axis of (183.0°, 69°) and (350.0°, 69°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.06 and an inclination of 2° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Kitt Peak in December 1996. Between 1900 and 2200 its closest approach with Earth is more than 0.11 AU.
The analysis of Rosetta images in combination with photometric light curves yielded the position of the north rotational pole of Lutetia: , . This gives an axial tilt of 96° (retrograde rotator), meaning that the axis of rotation is approximately parallel to the ecliptic, similar to the planet Uranus.
In March 2019, whurley and Mike Erwin formed the venture capital firm Ecliptic Capital, a $125 million fund to invest in the Austin tech scene. Five startups that they have invested in will be rolled into the fund: SoftMatch, Sempulse, Patchr.io, Unchained Capital, and whurley's own Strangeworks.
Its orbit has an eccentricity of 0.11 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Kitt Peak in April 1998. Between 1900 and 2200 its closest approach to Earth is more than 0.14 AU.
Kamoʻoalewa orbits the Sun at a distance of 0.90–1.10 AU once every 366 days. Its orbit has an eccentricity of 0.10 and an inclination of 8° with respect to the ecliptic. It has an Earth minimum orbital intersection distance of which translates into 13.6 lunar distances.
Although the zodiac remains the basis of the ecliptic coordinate system in use in astronomy besides the equatorial one,Shapiro, Lee T. "Constellations in the zodiac." NASA. 27 April 2011. the term and the names of the twelve signs are today mostly associated with horoscopic astrology.
Its orbit has an eccentricity of 0.06 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins with a precovery taken at the Siding Spring Observatory in July 1982, more than 15 years prior to its official discovery observation at Xinglong.
Is this Copernicus coming back to haunt us? That's crazy. > We're looking out at the whole universe. There's no way there should be a > correlation of structure with our motion of the earth around the sun – the > plane of the earth around the sun – the ecliptic.
A modeled lightcurve using photometric data from the Lowell Photometric Database and from the Wide-field Infrared Survey Explorer (WISE) was published in 2018. It gave a divergent sidereal period of hours and includes two spin axes at (172.0°, 20.0°) and (352.0°, 42.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.19 and an inclination of 12° with respect to the ecliptic. Itha was first observed as () at the U.S. Taunton Observatory in Massachusetts. The body's observation arc begins at Heidelberg Observatory on 23 August 1919, the night after its official discovery observation.
In 2013, an international study modeled a lightcurve from various data sources including the Uppsala Asteroid Photometric Catalogue and the Palomar Transient Factory survey. The modeling gave a concurring period of 8.79079 hours and determined two spin axis in ecliptic coordinates (λ, β) of: (357.0°, −49.0°) and (161.0°, −60.0°).
Its orbit has an eccentricity of 0.15 and an inclination of 6° with respect to the ecliptic. In 1917, it was first observed as at Simeiz Observatory (and Heidelberg on the following night), extending the body's observation arc by 12 years prior to its official discovery observation at Heidelberg.
The Kozai mechanism is capable of transferring orbital eccentricity to a higher inclination. The object is also the largest possible dwarf planet that has an inclination larger than 45°, traveling further "up and down" than "left to right" around the Sun when viewed edge-on along the ecliptic.
Based upon parallax measurements from the Hipparcos mission, it is roughly from Earth. It is 1.8 degrees south of the ecliptic. Theta Ophiuchi appears to be a triple star system. The brightest component is a spectroscopic binary with an orbital period of 56.71 days and an eccentricity of 0.17.
249 An eclipse can occur when the Moon's orbit crosses the ecliptic. This happens twice a year and is referred to as the ascending or descending node. An eclipse can occur during a period 18 days before or after an ascending or descending node. This is an Eclipse season.
Torquetum The torquetum or turquet is a medieval astronomical instrument designed to take and convert measurements made in three sets of coordinates: Horizon, equatorial, and ecliptic. It is said to be a combination of Ptolemy's astrolabon and the plane astrolabe. In a sense, the torquetum is an analog computer.
The rete, representing the sky, functions as a star chart. When it is rotated, the stars and the ecliptic move over the projection of the coordinates on the tympan. One complete rotation corresponds to the passage of a day. The astrolabe is, therefore, a predecessor of the modern planisphere.
Modeled photometric data from the Lowell Photometric Database (LPD) and the robotic BlueEye600 Observatory, gave a concurring period of 5.57556 and 5.57557 hours, respectively. Both studies determined two spin axes of (72.0°, −66.0°) and (241.0°, −66.0°), as well as (61.0°, −2.0°) and (223.0°, −68.0°) in ecliptic coordinates (λ, β).
Terentia orbits the Sun at a distance of 2.6–3.3 AU once every 5.01 years (1,832 days). Its orbit has an eccentricity of 0.12 and an inclination of 10° with respect to the ecliptic. The body's observation arc begins at Simeiz, 5 days after its official discovery observation.
Pisces is a constellation of the zodiac and is located in the Northern celestial hemisphere. Its name is the Latin plural for fish. It lies between Aquarius to the west and Aries to the east. The ecliptic and the celestial equator intersect within this constellation and in Virgo.
In addition to the rotational pole, a planet's orbit also has a defined direction in space. The direction of the angular momentum vector of that orbit can be defined as an orbital pole. Earth's orbital pole, i.e. the ecliptic pole, points in the direction of the constellation Draco.
JPL's small body data base shows this object having an aphelion distance of 39.2 AU, whereas the Deep Ecliptic Survey (DES) finds an aphelion distance of 91 AU, which would make it a trans-Neptunian object by JPL's orbital classification (hence the uncertainty whether is a centaur at all).
Orbital inclination and rotation. # The Moon has a 1:1 spin–orbit resonance. This means that the rotation–orbit ratio of the Moon is such that the same side of it always faces the Earth. # The Moon's rotational axis maintains a constant angle of inclination from the ecliptic plane.
Its orbit has an eccentricity of 0.95 and an inclination of 119° with respect to the ecliptic. The body's observation arc begins with a precovery taken by Astrovirtel at ESO's La Silla Observatory in February 2001, or 19 months prior to its official discovery observation at Anderson Mesa.
Because nutation causes a change to the frame of reference, rather than a change in position of an observed object itself, it applies equally to all objects. Its magnitude at any point in time is usually expressed in terms of ecliptic coordinates, as nutation in longitude (\Delta\psi) and nutation in obliquity (\Delta\epsilon). The largest term in nutation is expressed numerically (in arcseconds) as follows: :\Delta\psi = -17.2\sin\Omega :\Delta\epsilon = 9.2\cos\Omega where \Omega is the ecliptic longitude of the ascending node of the Moon's orbit. By way of reference, the sum of the absolute value of all the remaining terms is 1.4 arcseconds for longitude and 0.9 arcseconds for obliquity.
The main reason is that during the time that the Moon has completed an orbit around the Earth, the Earth (and Moon) have completed about of their orbit around the Sun: the Moon has to make up for this in order to come again into conjunction or opposition with the Sun. Secondly, the orbital nodes of the Moon precess westward in ecliptic longitude, completing a full circle in about 18.60 years, so a draconic month is shorter than a sidereal month. In all, the difference in period between synodic and draconic month is nearly days. Likewise, as seen from the Earth, the Sun passes both nodes as it moves along its ecliptic path.
On February 8, 1992, the Ulysses solar probe flew past Jupiter's north pole at a distance of 451,000 km. This swing-by maneuver was required for Ulysses to attain a very high-inclination orbit around the Sun, increasing its inclination to the ecliptic to 80.2 degrees. The giant planet's gravity bent the spacecraft's flightpath downward and away from the ecliptic plane, placing it into a final orbit around the Sun's north and south poles. The size and shape of the probe's orbit were adjusted to a much smaller degree, so that its aphelion remained at approximately 5 AU (Jupiter's distance from the Sun), while its perihelion lay somewhat beyond 1 AU (Earth's distance from the Sun).
The outer boundary of the heliosheath is called the heliopause, which is where the spacecraft are headed now. This is the region where the Sun's influence begins to decrease and interstellar space can be detected. Voyager 1 is escaping the Solar System at the speed of 3.6 AU per year 35° north of the ecliptic in the general direction of the solar apex in Hercules, while Voyager 2s speed is about 3.3 AU per year, heading 48° south of the ecliptic. The Voyager spacecraft will eventually go on to the stars. In about 40,000 years, Voyager 1 will be within 1.6 light years (ly) of AC+79 3888, also known as Gliese 445, which is approaching the Sun.
20, 28 In order to fix the exact primary direction, these motions necessitate the specification of the equinox of a particular date, known as an epoch, when giving a position. The three most commonly used are: ; Mean equinox of a standard epoch (usually J2000.0, but may include B1950.0, B1900.0, etc.): is a fixed standard direction, allowing positions established at various dates to be compared directly. ; Mean equinox of date: is the intersection of the ecliptic of "date" (that is, the ecliptic in its position at "date") with the mean equator (that is, the equator rotated by precession to its position at "date", but free from the small periodic oscillations of nutation). Commonly used in planetary orbit calculation.
The orbit of the Moon lies in a plane that is inclined about 5.14° with respect to the ecliptic plane. The line of intersection of these planes passes through the two points at which the Moon's orbit crosses the ecliptic plane: the ascending node, where the Moon enters the Northern Celestial Hemisphere, and the descending node, where the Moon moves into the Southern. The draconic or nodical month is the average interval between two successive transits of the Moon through the same node. Because of the torque exerted by the Sun's gravity on the angular momentum of the Earth-Moon system, the plane of the Moon's orbit gradually rotates westward, which means the nodes gradually rotate around Earth.
Axial precession is the movement of the rotational axis of an astronomical body, whereby the axis slowly traces out a cone. In the case of Earth, this type of precession is also known as the precession of the equinoxes, lunisolar precession, or precession of the equator. Earth goes through one such complete precessional cycle in a period of approximately 26,000 years or 1° every 72 years, during which the positions of stars will slowly change in both equatorial coordinates and ecliptic longitude. Over this cycle, Earth's north axial pole moves from where it is now, within 1° of Polaris, in a circle around the ecliptic pole, with an angular radius of about 23.5°.
Animation showing Orion's proper motion from 50000 BC to 50000 AD. Pi3 Orionis moves the most rapidly. Orion is located on the celestial equator, but it will not always be so located due to the effects of precession of the Earth's axis. Orion lies well south of the ecliptic, and it only happens to lie on the celestial equator because the point on the ecliptic that corresponds to the June solstice is close to the border of Gemini and Taurus, to the north of Orion. Precession will eventually carry Orion further south, and by AD 14000 Orion will be far enough south that it will become invisible from the latitude of Great Britain.
After the first roll the spacecraft had no problem in reorienting itself with Alpha Centauri, Voyager 1's guide star, and it resumed sending transmissions back to Earth. Voyager 1 was expected to enter interstellar space "at any time". Voyager 2 was still detecting outward flow of solar wind at that point but it was estimated that in the following months or years it would experience the same conditions as Voyager 1. The spacecraft was reported at 12.44° declination and 17.163 hours right ascension, and at an ecliptic latitude of 34.9° (the ecliptic latitude changes very slowly), placing it in the constellation Ophiuchus as observed from the Earth on May 21, 2011.
Ulysses second orbit (1999–2004) Animation of Ulysses trajectory from October 6, 1990 to June 29, 2009 It arrived at Jupiter on February 8, 1992 for a swing-by maneuver that increased its inclination to the ecliptic by 80.2 degrees. The giant planet's gravity bent the spacecraft's flight path southward and away from the ecliptic plane. This put it into a final orbit around the Sun that would take it past the Sun's north and south poles. The size and shape of the orbit were adjusted to a much smaller degree so that aphelion remained at approximately 5 AU, Jupiter's distance from the Sun, and perihelion was somewhat greater than 1 AU, the Earth's distance from the Sun.
Based upon photometry observations between 1984−2007, it has a sidereal rotation period of 8.283065 h with an amplitude that can range up to in magnitude. The lightcurve shows some shape irregularities. There are two valid solutions for the pole's ecliptic coordinates: (λ1, β1) = (38°, +75°) and (λ2, β2) = (237°, +73°).
Alvema orbits the Sun in the central main-belt at a distance of 1.9–3.7 AU once every 4 years and 8 months (1,698 days). Its orbit has an eccentricity of 0.31 and an inclination of 7° with respect to the ecliptic. No precoveries were taken prior to its discovery.
Betulia orbits the Sun at a distance of 1.1–3.3 AU once every 3 years and 3 months (1,190 days). Its orbit has an eccentricity of 0.49 and an inclination of 52° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Johannesburg in 1950.
Photometric and radiometric observations of Betulia were also used to model the asteroid's lightcurve. It gave a concurring period of 6.13836 hours as well as a spin axis of (133.0°, 22.0°) and (136.0°, 22.0°) in ecliptic coordinates (λ, β), respectively. The results supersede previously determined rotational poles (also see LCDB summary).
Makharadze belongs to the Nysa family of asteroids. It orbits the Sun in the inner main-belt at a distance of 2.0–2.9 AU once every 3 years and 10 months (1,411 days). Its orbit has an eccentricity of 0.19 and an inclination of 2° with respect to the ecliptic.
Marsden is a member of the Hilda family. It orbits the Sun in the outermost main-belt at a distance of 3.1–4.8 AU once every 7 years and 10 months (2,861 days). Its orbit has an eccentricity of 0.21 and an inclination of 18° with respect to the ecliptic.
Atlantis orbits the Sun at a distance of 1.5–3.0 AU once every 3 years and 5 months (1,233 days). Its orbit has an eccentricity of 0.34 and an inclination of 3° with respect to the ecliptic. The asteroids's observation arc begins at Heidelberg one week after its official discovery observation.
Its orbit has an eccentricity of 0.12 and an inclination of 6° with respect to the ecliptic. The asteroid was first identified as at Simeiz Observatory in September 1915. Its observation arc begins at Algiers Observatory in August 1930, more than a year after its official discovery observation at Uccle.
Kepler orbits the Sun at a distance of 1.4–3.9 AU once every 4 years and 5 months (1,601 days). Its orbit has an eccentricity of 0.47 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins at Heidelberg, the night after its official discovery observation.
The armillary sphere has three sets of rings that represent the celestial sphere. The first group contains fixed meridian, horizon, and equatorial rings. The second group contains ecliptic, solstitial, and equinoctial rings that turn as a unit. The inner group contains one meridian ring that moves around the celestial pole.
360 Carlova is a very large main-belt asteroid. It is classified as a C-type asteroid and is probably composed of carbonaceous material. The asteroid has a convex, roughly ellipsoid shape. The sidereal rotation period is 6.1873 hours with an axis of rotation along the ecliptic coordinates (l, b) = (, ).
Columbia orbits the Sun at a distance of 2.6–2.9 AU once every 4 years and 8 months (1,691 days). Its orbit has an eccentricity of 0.06 and an inclination of 7° with respect to the ecliptic. The body's observation arc begins the night after its official discovery at Nice.
Its orbit has an eccentricity of 0.90 and an inclination of 160° with respect to the ecliptic. Its observation arc begins 12 months prior to its official discovery observation, with a precovery taken by Spacewatch at Steward Observatory in June 1998. Currently, its orbit still has an uncertainty of 2.
It is not clear however whether the Arabic names derived from the earlier Coptic forms, or whether the Coptic terms were themselves borrowed from the Arabic. Kircher asserted that the Ancient Egyptian names, preserved in Coptic, formed the basis of Babylonian and Indian names for the same equinoctial-ecliptic stars.
It may have formed from debris knocked off Phoebe. The Thrymian orbit is retrograde, at an inclination of 175° to the ecliptic (151° to Saturn's equator) and with an eccentricity of 0.453. Its rotation period is hours. Its name was announced in its oblique form Thrym in IAU Circular 8177.
In 2016, a modeled lightcurve using photometric data from various sources was published. It gave a concurring period of 97.278 hours, as well as a spin axis of (236.0°, 75.0°) in ecliptic coordinates (λ, β). All lightcurve observations show a high brightness variation, indicative for an elongated, non-spheroidal shape.
Using 160 observations over 43 days, Charles J. Merfield (1866–1931) could calculate only a parabolic orbit, inclined about 131° to the ecliptic. The comet travelled in a retrograde orbit relative to the planetary orbits. The comet was on April 10 about .56 AU from Venus and on April 21 about .
This yields numerical values for the Moon's secular deceleration, i.e. negative acceleration, in longitude and the rate of change of the semimajor axis of the Earth–Moon ellipse. From the period 1970–2012, the results are: : −25.82 ± 0.03 arcsecond/century2 in ecliptic longitudeJ.G. Williams, D.H. Boggs and W. M.Folkner (2013).
The nakshatras (or more precisely nákṣatra, lit. "stars") are the Indian form of lunar stations. They usually number 27 but sometimes 28 and their names are related to the most prominent constellations in each sector. They start from a point on the ecliptic precisely opposite the star Spica (Sanskrit: Chitrā) and develop eastwards.
Its orbit has an eccentricity of 0.14 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with an observation made by the space-based Wide-field Infrared Survey Explorer on 22 July 2017, one day after its close flyby and a day before its official first observation.
Minor planet 1722 Goffin orbits the Sun at a distance of 2.4–2.6 AU once every 3 years and 12 months (1,456 days). Its orbit has an eccentricity of 0.05 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins 6 days after its official discovery observation.
The C-type asteroid orbits the Sun in the central main-belt at a distance of 2.2–3.2 AU once every 4 years and 4 months (1,597 days). Its orbit has an eccentricity of 0.19 and an inclination of 19° with respect to the ecliptic. No precoveries were taken before its discovery.
In 2011 and 2013, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources was published. In both studies, the modeled lightcurve gave a concurring period 9.9586 hours. The 2013-publication also determined two spin axis of (170.0°, −86.0°) and (27.0°, −61.0°) in ecliptic coordinates (λ, β) ().
Lucidor has not been grouped to any known asteroid family. It orbits the Sun in the central main belt at a distance of 2.3–3.1 AU once every 4 years and 5 months (1,613 days). Its orbit has an eccentricity of 0.14 and an inclination of 7° with respect to the ecliptic.
In 2013, an international study modeled a lightcurve from various data sources including the Uppsala Asteroid Photometric Catalogue and the Palomar Transient Factory survey. The lightcurve gave a concurring period of 18.2183 hours and allowed for the determination of two spin axis of (32.0°, 74.0°) and (197.0°, 65.0°) in ecliptic coordinates (λ, β).
In 2013, an international study modeled a lightcurve from various data sources including the Uppsala Asteroid Photometric Catalogue and the Palomar Transient Factory survey. The lightcurve gave a concurring period of 5.25047 hours and allowed for the determination of two spin axis of (62.0°, 60.0°) and (265.0°, 45.0°) in ecliptic coordinates (λ, β).
Its orbit has an eccentricity of 0.09 and an inclination of 17° with respect to the ecliptic. The body's observation arc begins with a precovery published by the Digitized Sky Survey and taken at Palomar Observatory in November 1989, more than 6 years prior to its official discovery observation at La Silla.
Ithaka is a non-family asteroid from the background population. It orbits the Sun in the inner main-belt at a distance of 1.7–3.1 AU once every 3 years and 9 months (1,364 days). Its orbit has an eccentricity of 0.28 and an inclination of 7° with respect to the ecliptic.
The Maya identified 13 constellations along the ecliptic. These are the content of an almanac in the Paris Codex. Each of these was associated with an animal. These animal representations are pictured in two almanacs in the Madrid Codex where they are related to other astronomical phenomena – eclipses and Venus – and Haab rituals.
It orbits the Sun at a distance of 1.0–1.7 AU once every 1 years and 7 months (585 days; semi-major axis of 1.37 AU). Its orbit has an eccentricity of 0.27 and an inclination of 9° with respect to the ecliptic. is a V-type asteroid with a bright surface.
The asteroid orbits the Sun at a distance of 0.9–4.0 AU once every 3 years and 10 months (1,388 days). Its orbit has an eccentricity of 0.64 and an inclination of 68° with respect to the ecliptic. No precoveries were taken. The asteroid's observation arc even begins 2 days after its discovery.
In 2016, a lightcurve of Salonta has also been modeled using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and from individual observers. Modelling gave a concurring sidereal period of 8.86985 hours as well as two spin axis of (223.0°, 18.0°) and (57.0°, 35°) in ecliptic coordinates (λ, β).
In 2013, an international study modeled a lightcurve from various data sources including the Uppsala Asteroid Photometric Catalogue and the Palomar Transient Factory survey. The lightcurve gave a sidereal period of 29.4674 hours and allowed for the determination of two spin axis of (156.0°, −4.0°) and (338.0°, 15.0°) in ecliptic coordinates (λ, β).
Gemini later gained the ability to expand its form where it grows in size and gains super-strength. In its second form, Gemini can fly and release blasts of energy. Gemini in this form also exhibited a talkative personality. The Ecliptic Gemini that served as Madison Jeffries' "twin" did not demonstrate any powers.
' orbits the Sun at a distance of 11.1–31.2 AU once every 97 years and 2 months (35,473 days; semi-major axis of 21.13 AU). Its orbit has an eccentricity of 0.47 and an inclination of 100° with respect to the ecliptic. The body's observation arc begins at Pan-STARRS in June 2010.
The celestial equator is divided into twelve, and these divisions are projected on to the ecliptic along great circles that take in the north and south points on the horizon. Named after the German astronomer and astrologer Johann Müller of Königsberg. The Regiomontanus system was later largely replaced by the Placidus system.
In two separate studies, groups of German, Russian and Swedish astronomers also modeled Venetias lightcurve from various data sources in 2000 and 2002. They found two spin axes of (259.0°, −30.0°) and (268.0°, −24.0°) in ecliptic coordinates (λ, β), as well as a concurring rotation period of 13.33170 and 13.34153 hours, respectively ().
K2-72 also has the 2MASS catalogue number J22182923-0936444. Its EPIC (Ecliptic Plane Input Catalog) number is 206209135. The star's planetary companions were discovered by NASA's Kepler Mission, a mission tasked with discovering planets in transit around their stars. The transit method that Kepler uses involves detecting dips in brightness in stars.
276, No. 1257, The Place of Astronomy in the Ancient World (May 2, 1974), pp. 6782. Accessed 9 Oct 2012. The Twenty-Eight Mansions form an ecliptic coordinate system used for those stars visible (from China) but not during the whole year, based on the movement of the moon over a lunar month.
The first is separated by 0.1 arcseconds, or at least 13 AUs. The second is 0.4 arcseconds away, which is 40 AU or more. Nothing is known about the orbits of these stars. Being 1.43 degrees north of the ecliptic, Pi Sagittarii can be occulted by the Moon, and, very rarely, by planets.
Diagram of a Class C Stellar Engine—to scale—built around a Sun-like star. It consists of a partial Dyson swarm composed of 5 Dyson Rings of solar collectors (the Class B component), and a large statite Shkadov thruster (the Class A component). Perspective is from below the system's ecliptic at a distance of ~2.8 AU. The system's direction of acceleration is on a vector which passes from the center of the star through the center of the Shkadov thruster, which is hovering over the star's north pole (with regards to the ecliptic), at a distance of 1 AU. Stellar engines are a class of hypothetical megastructures which use a star's radiation to create usable energy. The concept has been introduced by Badescu and Cathcart.
Dust in the Kuiper belt creates a faint infrared disc. (Click on the "play" button to watch the video.) At its fullest extent (but excluding the scattered disc), including its outlying regions, the Kuiper belt stretches from roughly 30–55 AU. The main body of the belt is generally accepted to extend from the 2:3 mean-motion resonance (see below) at 39.5 AU to the 1:2 resonance at roughly 48 AU. The Kuiper belt is quite thick, with the main concentration extending as much as ten degrees outside the ecliptic plane and a more diffuse distribution of objects extending several times farther. Overall it more resembles a torus or doughnut than a belt. Its mean position is inclined to the ecliptic by 1.86 degrees.
Pallas has a high eccentricity and a highly inclined orbit Pallas has unusual dynamic parameters for such a large body. Its orbit is highly inclined and moderately eccentric, despite being at the same distance from the Sun as the central part of the asteroid belt. Furthermore, Pallas has a very high axial tilt of 84°, with its north pole pointing towards ecliptic coordinates (β, λ) = (30°, −16°) with a 5° uncertainty in the Ecliptic J2000.0 reference frame. This means that every Palladian summer and winter, large parts of the surface are in constant sunlight or constant darkness for a time on the order of an Earth year, with areas near the poles experiencing continuous sunlight for as long as two years.
If this had not happened, the Moon would now lie much closer to the ecliptic and eclipses would be much more frequent. The rotational axis of the Moon is not perpendicular to its orbital plane, so the lunar equator is not in the plane of its orbit, but is inclined to it by a constant value of 6.688° (this is the obliquity). As was discovered by Jacques Cassini in 1722, the rotational axis of the Moon precesses with the same rate as its orbital plane, but is 180° out of phase (see Cassini's Laws). Therefore, the angle between the ecliptic and the lunar equator is always 1.543°, even though the rotational axis of the Moon is not fixed with respect to the stars.
Where the hands representing the Sun and the Moon cut across the outer rim of this circle, is where the Sun and Moon are currently visible within the ecliptic. The twelve symbols decorating the circle are the twelve signs of the zodiac; it is thus possible to determine which of the twelve constellations the Sun or Moon lies in front of at any given moment. The red and black fields at the bottom of the clock phase represent the horizon, as observable from Lund Cathedral. If the point where the hand representing the sun cuts the outer rim of the circle depicting the ecliptic, and that point is over the black field, it means the sun is below the horizon and it is night.
Thus the Milky Way, especially rich in the area of Cygnus, is always visible from the northern hemisphere. The South celestial pole is correspondingly found at and , which is a couple of degrees from the 2.5-magnitude star Kappa Velorum (which is at ), which could therefore be considered the southern polar star. The star Canopus, second-brightest in the sky, is a circumpolar star for most southern latitudes. The zodiac constellations of Mars's ecliptic are almost the same as those of Earth -- after all, the two ecliptic planes only have a mutual inclination of 1.85° -- but on Mars, the Sun spends 6 days in the constellation Cetus, leaving and re-entering Pisces as it does so, making a total of 14 zodiacal constellations.
The Moon differs from most natural satellites around other planets in that it remains near the ecliptic (the plane of Earth's orbit around the Sun) instead of Earth's equatorial plane. The Moon's maximum and minimum declination vary because the plane of the Moon's orbit around Earth is inclined about 5.14° with respect to the ecliptic plane, and the spatial direction of the Moon's orbital inclination gradually changes over an 18.6-year cycle, alternately adding to or subtracting from the 23.5° tilt of Earth's axis. Therefore, the maximum declination of the Moon varies roughly from (23.5° − 5° =) 18.5° to (23.5° + 5° =) 28.5°. At the minor lunar standstill, the Moon will change its declination during the nodal period from +18.5° to −18.5°, for a total range of 37°.
The spacecraft spin axis was normal to the ecliptic plane, and its spin rate was 5 rpm, with propulsion Star-17A. The initial apogee point lay near the earth-sun line. The solar-cell and chemical-battery powered spacecraft carried 2 transmitters. One continuously transmitted PCM encoder data at a 1,600 bps information bit rate.
Two lightcurves, published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring sidereal period of and hours, respectively. Each modeled lightcurve also determined two spin axes of (68.0°, 58.0°) and (253.0°, 61.0°), as well as (262.0°, 71.0°) and (47.0°, 66.0°) in ecliptic coordinates (λ, β).
Two lightcurves, published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring sidereal period of and hours, respectively. Each modeled lightcurve also determined two spin axes of (123.0°, −58.0°) and (337.0°, −47.0°), as well as (115.0°, −77.0°) and (338.0°, −43.0°) in ecliptic coordinates (λ, β).
Aidamina is a non-family asteroid from the main belt's background population. It orbits the Sun in the outer asteroid belt at a distance of 2.4–3.9 AU once every 5 years and 9 months (2,089 days). Its orbit has an eccentricity of 0.23 and an inclination of 22° with respect to the ecliptic.
Campestris is a non-family asteroid from the main belt's background population. It orbits the Sun in the central main-belt at a distance of 2.1–3.2 AU once every 4 years and 5 months (1,612 days). Its orbit has an eccentricity of 0.20 and an inclination of 3° with respect to the ecliptic.
Two of the reaction wheels of spacecraft failed, so the engineers made a better and smarter plan to redesign the mission. K2 mission was still searching for exoplanets and different planets in the space however it was doing it different way, it was scanning a larger swath of sky than before along with ecliptic plane.
Two lightcurves, published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring sidereal period of and hours, respectively. Each modeled lightcurve also determined two spin axes of (104.0°, −57.0°) and (267.0°, −53.0°), as well as (294.0°, −60.0°) and (157.0°, −57.0°) in ecliptic coordinates (λ, β), respectively.
Bistro orbits the Sun in the inner main-belt at a distance of 2.2–2.7 AU once every 3 years and 10 months (1,388 days). Its orbit has an eccentricity of 0.09 and an inclination of 15° with respect to the ecliptic. The asteroid's observation arc begins with its official discovery observation at Zimmerwald.
The asteroid orbits the Sun at a distance of 1.3–1.5 AU once every 20 months (599 days). Its orbit has an eccentricity of 0.06 and an inclination of 39° with respect to the ecliptic. Licks observation arc begins with its discovery observation, as no precoveries were taken, and no prior identifications were made.
Its orbit has an eccentricity of 0.13 and an inclination of 5° with respect to the ecliptic. The asteroid was first observed at Goethe Link Observatory in October 1952. The body's observation arc begins with its observation as at Crimea-Nauchnij in August 1966, more than 15 years prior to its official discovery observation.
In astrology, the Equatorial Ascendant, or the East Point, is the sign and degree rising over the Eastern Horizon at the Earth's equator at any given time. In the celestial sphere it corresponds to the intersection of the ecliptic with a great circle containing the celestial poles and the East point of the horizon.
Asaph orbits the Sun in the outer main-belt at a distance of 2.1–3.7 AU once every 4 years and 11 months (1,781 days). Its orbit has an eccentricity of 0.28 and an inclination of 22° with respect to the ecliptic. The asteroid's observation arc begins with its official discovery observation Goethe Link.
' orbits the Sun at a distance of 0.7–1.2 AU once every 11 months (338 days; semi-major axis of 0.95 AU). Its orbit has an eccentricity of 0.28 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Catalina Station in September 2006.
Kassite Period ( 1600—1155 BCE). The original Eanna temple in Uruk was first dedicated to Anu, but later dedicated to Inanna. In Mesopotamian religion, Anu was the personification of the sky, the utmost power, the supreme god, the one "who contains the entire universe". He was identified with the north ecliptic pole centered in Draco.
Its orbit has an eccentricity of 0.24 and an inclination of 1° with respect to the ecliptic. The asteroid was first observed as at Turku Observatory in February 1944. The body's observation arc begins with its observation as at Heidelberg Observatory in October 1949, fifteen months prior to its official discovery observation at Goethe Link.
Ryugu orbits the Sun at a distance of 0.96–1.41 au once every 16 months (474 days; semi-major axis of 1.19 au). Its orbit has an eccentricity of 0.19 and an inclination of 6° with respect to the ecliptic. It has a minimum orbital intersection distance with Earth of , equivalent to 0.23 lunar distances.
The angular resolutions are 22.5° × 36° for the SST and 5.6° (near the ecliptic) to 22.5° for the top-hat ES analyzers. The particle detectors can obtain a full 4π steradian coverage in one full(half) spin (~3 s) for the SST (top-hat ES analyzers). The majority of this section was taken from.
The asteroid is a background asteroid, that is not a member of any known asteroid family. Sakuntala orbits the Sun in the central main-belt at a distance of 2.0–3.1 AU once every 4.04 years (1,474 days). Its orbit has an eccentricity of 0.21 and an inclination of 19° with respect to the ecliptic.
Suthers is a non-family asteroid from the main belt's background population. It orbits the Sun in the inner main-belt at a distance of 2.1–2.5 AU once every 3 years and 6 months (1,263 days). Its orbit has an eccentricity of 0.09 and an inclination of 4° with respect to the ecliptic.
The asteroid orbits the Sun in the central main- belt at a distance of 2.0–3.6 AU once every 4 years and 8 months (1,694 days). Its orbit has an eccentricity of 0.29 and an inclination of 17° with respect to the ecliptic. Walbecks observation arc begins the night after its official discovery observation.
Mozartia orbits the Sun in the inner main-belt at a distance of 1.7–2.9 AU once every 3 years and 6 months (1,268 days). Its orbit has an eccentricity of 0.26 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins with its official discovery observation in 1924.
Philoctetes orbits in the Lagrangian point of the Sun–Jupiter system, in the "Greek Camp" of Trojan asteroids. It orbits the Sun at a distance of 4.9–5.6 AU once every 11 years and 11 months (4,353 days). Its orbit has an eccentricity of 0.07 and an inclination of 4° with respect to the ecliptic.
Davidweilla orbits the Sun in the inner main-belt at a distance of 1.8–2.7 AU once every 3 years and 5 months (1,237 days). Its orbit has an eccentricity of 0.19 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Algiers.
Amazone orbits the Sun in the outer main-belt at a distance of 3.0–3.5 AU once every 5 years and 10 months (2,131 days). Its orbit has an eccentricity of 0.09 and an inclination of 21° with respect to the ecliptic. The body's observation arc begins three weeks after its official discovery observation.
In celestial mechanics true longitude is the ecliptic longitude at which an orbiting body could actually be found if its inclination were zero. Together with the inclination and the ascending node, the true longitude can tell us the precise direction from the central object at which the body would be located at a particular time.
Its orbit has an eccentricity of 0.07 and an inclination of 14° with respect to the ecliptic. The asteroid was first observed at Palomar Observatory in August 1952. One year later, the body's observation arc begins at Palomar in August 1953, or more than 36 years prior to its official discovery observation at Cerro Tololo.
Utra is a S-type asteroid. It orbits the Sun in the central main-belt at a distance of 2.4–2.6 AU once every 4.04 years (1,474 days). Its orbit has an eccentricity of 0.04 and an inclination of 5° with respect to the ecliptic. Utra was first identified as at Heidelberg Observatory in 1918.
Transylvania is a non-family asteroid of the main belt's background population. It orbits the Sun in the outer main-belt at a distance of 2.1–4.0 AU once every 5 years and 4 months (1,947 days). Its orbit has an eccentricity of 0.30 and an inclination of 4° with respect to the ecliptic.
Leo wore a lion-skin costume equipped with claws on his costume's "paws" as weapons. The Android Leo has super human strength, agility, endurance, a set of razor sharp claws, enhanced hearing and vision. The female Android Leo had the same abilities as Tigra. The Ecliptic Leo possessed superhuman strength, besides using claws and fangs.
Astronomical data are often specified not only in their relation to an epoch or date of reference but also in their relations to other conditions of reference, such as coordinate systems specified by "equinox", or "equinox and equator", or "equinox and ecliptic" - when these are needed for fully specifying astronomical data of the considered type.
In 2016, two modeled lightcurves using photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring period of 23.4827 and 23.4830 hours, respectively. Each modeled lightcurve also determined two spin axis of (139.0°, −58.0°) and (330.0°, −81.0°), as well as (7.0°, −54.0°) and (168.0°, −56.0°) in ecliptic coordinates (λ, β), respectively.
Two lightcurves, published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring period of () and () hours, respectively. Each modeled lightcurve also determined two spin axes of (92°, 66°) and (244°, 54°), as well as (91°, 70°) and (250°, 45°) in ecliptic coordinates (λ, β), respectively.
Two lightcurves, published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring sidereal period of () and () hours, respectively. Each modeled lightcurve also determined two spin axes of (213.0°, −66.0°) and (76.0°, −49.0°), as well as (282.0°, −79.0°) and (114.0°, −45.0°) in ecliptic coordinates (λ, β), respectively.
Two lightcurves, published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring sidereal period of () and () hours, respectively. Each modeled lightcurve also determined two spin axes of (93.0°, −71.0°) and (277.0°, −35.0°), as well as (56.0°, −78.0°) and (255.0°, −57.0°) in ecliptic coordinates (λ, β), respectively.
Rotational lightcurves obtained from photometric observations gave a rotation period of 3.423 hours (best result) with a brightness variation between 0.13 and 0.27 magnitude (). Radar observations gave a concurring period of 3.4256 hours, and subsequent modeling of both radiometric and photometric observations gave a spin axis of (309.0°, −80.0°) in ecliptic coordinates (λ, β).
A satellite is said to occupy an inclined orbit around Earth if the orbit exhibits an angle other than 0° to the equatorial plane. This angle is called the orbit's inclination. A planet is said to have an inclined orbit around the Sun if it has an angle other than 0° to the ecliptic plane.
The star system has a combined apparent magnitude of 2.9. The system is 39 light years away from the Sun. Gamma Virginis is 2.8 degrees north of the ecliptic, so it can be occulted by the Moon and (rarely) by planets. In June 2011 Saturn passed a quarter of a degree south of Porrima.
It orbits the Sun at a distance of 0.7–0.9 AU once every 9 months (271 days; semi-major axis of 0.82 AU). Its orbit has an eccentricity of 0.15 and an unusually high inclination of 50° with respect to the ecliptic. The orbital evolution of leads the object into the Aten orbital realm periodically.
Caju orbits the Sun at a distance of 35.2–821 AU once every 8856 years (3,234,488 days; semi-major axis of 428 AU). Its orbit has an exceptionally high eccentricity of 0.92 and an inclination of 54° with respect to the ecliptic. This makes it a probable outlier among the known extreme trans-Neptunian objects.
Grotius orbits the Sun in the central main-belt at a distance of 2.1–3.0 AU once every 4 years and 2 months (1,518 days). Its orbit has an eccentricity of 0.18 and an inclination of 7° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Palomar.
Vicia is a non-family asteroid from the main belt's background population. It orbits the Sun in the central main belt at a distance of 1.9–3.4 AU once every 4 years and 4 months (1,570 days). Its orbit has an eccentricity of 0.29 and an inclination of 2° with respect to the ecliptic.
Figneria is a non-family asteroid of the main belt's background population. It orbits the Sun in the outer main belt at a distance of 2.3–4.1 AU once every 5 years and 8 months (2,071 days). Its orbit has an eccentricity of 0.28 and an inclination of 12° with respect to the ecliptic.
' orbits the Sun at a distance of 0.82–1.66 AU once every 17 months (503 days; semi-major axis of 1.24 AU). Its orbit has an eccentricity of 0.34 and an inclination of 9° with respect to the ecliptic. The asteroid has an Earth minimum orbital intersection distance of , which translates into 0.078 lunar distances.
Gould felt that the name had an "apt significance". The asteroid shares its name with Pandora, a moon of Saturn. This object is orbiting the Sun with a period of 4.58 years, a semimajor axis of , and an eccentricity of 0.14. Its orbital plane lies at an angle of 7.2° to the plane of the ecliptic.
Care must be taken to ensure the instrument isn't pointed directly towards the Sun because of the risk for eye damage. This method bypasses the limitation of twilight observing when the ecliptic is located at a low elevation (e.g. on autumn evenings). Ground-based telescope observations of Mercury reveal only an illuminated partial disk with limited detail.
The asteroid is orbiting the Sun with a period of , a semimajor axis of , and eccentricity of 0.165. The orbital plane is inclined by an angle of 8.59° to the plane of the ecliptic. Hesperia was observed by Arecibo radar in February 2010. Radar observations combined with lightcurve-based shape models, lead to a diameter estimate of .
Modeled photometric data from the Lowell Photometric Database (LPD) and WISE thermal data, gave a concurring sidereal rotation period of 8.57412 hours. Each modeled lightcurve also determined the object's spin axes. Durech gives only one pole, namely (7.0°, −59.0°), while Hanus determined two lower rated poles at (336.0°, −70.0°) and (72.0°, −56.0°) in ecliptic coordinates (λ, β).
Eupheme orbits Jupiter at an average distance of 19,622 Mm in 561.518 days, at an inclination of 146° to the ecliptic (146° to Jupiter's equator), in a retrograde direction and with an eccentricity of 0.2507. It belongs to the Ananke group, retrograde irregular moons that orbit Jupiter between 19.3 and 22.7 Gm, at inclinations of roughly 150°.
27 Piscium is a binary star system in the zodiac constellation of Pisces. It is visible to the naked eye with an apparent visual magnitude of 4.88. Based upon an annual parallax shift of , it is located about 234 light years away. The system is positioned near the ecliptic and so is subject to occultation by the Moon.
This happens when the Moon is near one of the two nodes of its orbit on the ecliptic at the time of the syzygy. Of course, to produce an eclipse, the Sun must also be near a node at that time: the same node for a solar eclipse, or the opposite node for a lunar eclipse.
22 Tauri is a component of the Asterope double star in the Pleiades open cluster. 22 Tauri is the stars' Flamsteed designation. It is situated near the ecliptic and thus is subject to lunar occultation. The star has an apparent visual magnitude of 6.43, which is near the lower threshold of visibility to the naked eye.
The star is situated near the ecliptic and thus is subject to lunar occultations. This is an aging K-type giant star with a stellar classification of K4III. Having exhausted the supply of hydrogen at its core, it has cooled and expanded off the main sequence. At present it has 41 times the girth of the Sun.
Hergenrother orbits the Sun in the outer main-belt at a distance of 2.3–3.5 AU once every 4 years and 11 months (1,786 days). Its orbit has an eccentricity of 0.20 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins 6 days after its official discovery observation at Turku.
It orbits the Sun at a distance of 1.9–2.8 AU once every 3 years and 6 months (1,278 days; semi-major axis of 2.31 AU). Its orbit has an eccentricity of 0.19 and an inclination of 23° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Palomar in May 1988.
Hanoi orbits the Sun in the inner main-belt at a distance of 1.6–3.0 AU once every 3 years and 6 months (1,287 days). Its orbit has an eccentricity of 0.29 and an inclination of 2° with respect to the ecliptic. No precoveries were taken. The asteroid's observation arc begins with its official discovery observation.
Hadwiger orbits the Sun at a distance of 2.4–2.7 AU once every 4 years and 1 month (1,497 days). Its orbit has an eccentricity of 0.06 and an inclination of 15° with respect to the ecliptic. It is a member of the Maria family of asteroids. In the Tholen classification, Hadwiger is a carbonaceous CSU-type.
Filatov orbits the Sun in the outer main-belt at a distance of 3.1–3.2 AU once every 5 years and 7 months (2,050 days). Its orbit has an eccentricity of 0.02 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins at Nauchnij, 2 days after its official discovery observation.
Dzus orbits the Sun in the central main-belt at a distance of 2.2–3.3 AU once every 4 years and 6 months (1,645 days). Its orbit has an eccentricity of 0.20 and an inclination of 16° with respect to the ecliptic. As no precoveries were taken, the asteroid's observation arc begins with its discovery observation in 1908.
Alfilipenko orbits the Sun in the outer main-belt at a distance of 2.7–3.8 AU once every 5 years and 10 months (2,132 days). Its orbit has an eccentricity of 0.17 and an inclination of 7° with respect to the ecliptic. No precoveries were taken. The asteroid's observation arc begins with its official discovery observation.
Corbin is a member of the Phocaea family (), a group of asteroids with similar orbital characteristics. It orbits the Sun in the inner main-belt at a distance of 1.9–2.9 AU once every 3 years and 7 months (1,324 days). Its orbit has an eccentricity of 0.21 and an inclination of 26° with respect to the ecliptic.
Clemence is a member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System. It orbits the Sun at a distance of 1.8–2.1 AU once every 2 years and 8 months (984 days). Its orbit has an eccentricity of 0.10 and an inclination of 19° with respect to the ecliptic.
Ostro is a member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System. It orbits the Sun at a distance of 1.8–2.0 AU once every 2 years and 7 months (950 days). Its orbit has an eccentricity of 0.07 and an inclination of 25° with respect to the ecliptic.
Komm orbits the Sun in the inner main- belt at a distance of 1.4–2.9 AU once every 3 years and 3 months (1,178 days). Its orbit has an eccentricity of 0.35 and an inclination of 6° with respect to the ecliptic. As no precoveries were taken, the asteroid's observation arc begins with its official discovery observation.
This asteroid is a member of the Phocaea family (), a group of asteroids with similar orbital characteristics. It orbits the Sun in the inner main-belt at a distance of 1.9–2.9 AU once every 3 years and 8 months (1,350 days). Its orbit has an eccentricity of 0.20 and an inclination of 23° with respect to the ecliptic.
Litva is a member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System. It orbits the Sun at a distance of 1.6–2.2 AU once every 2 years and 8 months (960 days). Its orbit has an eccentricity of 0.14 and an inclination of 23° with respect to the ecliptic.
The studies have also modeled the asteroid's lightcurve, using photometric data from the Lowell Photometric Database (LPD) and other sources. Modelling gave a concurring period of 4.566945 and 4.56695 hours, respectively. Each of the two studies also gave two spin axis in ecliptic coordinates (λ, β): (83.0°, −57°) and (270.0°, –62.0°), as well as (88.0°, −88°) and (267.0°, −66°).
Niels orbits the Sun in the inner main-belt at a distance of 2.0–2.4 AU once every 3 years and 3 months (1,182 days). Its orbit has an eccentricity of 0.10 and an inclination of 1° with respect to the ecliptic. First observed at Heidelberg in 1927, Niels observation arc begins with its official discovery observation in 1935.
Numerowia orbits the Sun in the outer main-belt at a distance of 2.7–3.0 AU once every 4 years and 10 months (1,771 days). Its orbit has an eccentricity of 0.05 and an inclination of 13° with respect to the ecliptic. The asteroid's observation arc begins at Heidelberg four days after its official discovery observation.
Chandra image showing Saturn's moon Titan transiting the nebula. The Crab Nebula lies roughly 1.5 degrees away from the ecliptic—the plane of Earth's orbit around the Sun. This means that the Moon—and occasionally, planets—can transit or occult the nebula. Although the Sun does not transit the nebula, its corona passes in front of it.
The YORP effect is typically considered for asteroids with their heliocentric orbit in the Solar System. The effect is responsible for the creation of binary and tumbling asteroids as well as for changing an asteroid's pole towards 0°, 90°, or 180° relative to the ecliptic plane and so modifying its heliocentric radial drift rate due to the Yarkovsky effect.
A rotational lightcurve analysis by Czech astronomer Petr Pravec in 2007 rendered a rotation period of hours with a high brightness amplitude of 1.13 in magnitude (). A modeled lightcurves using photometric data from various sources, gave a sidereal period of hours and two spin axes of (123.0°, −51.0°) and (314.0°, −60.0°) in ecliptic coordinates (λ, β).
Ohtsuka orbits the Sun in the inner main-belt at a distance of 1.8–3.1 AU once every 3 years and 11 months (1,416 days). Its orbit has an eccentricity of 0.26 and an inclination of 4° with respect to the ecliptic. First observed as at Heidelberg, the body's observation arc begins at Palomar in 1980.
Baillauda is a non-family asteroid from the main belt's background population. It orbits the Sun in the outer asteroid belt at a distance of 3.2–3.6 AU once every 6 years and 4 months (2,304 days; semi-major axis of 3.41). Its orbit has an eccentricity of 0.05 and an inclination of 6° with respect to the ecliptic.
Aster orbits the Sun in the inner main-belt at a distance of 2.0–2.5 AU once every 3 years and 5 months (1,244 days). Its orbit has an eccentricity of 0.11 and an inclination of 3° with respect to the ecliptic. The asteroid's observation arc begins at the discovering observatory, one week after its official discovery observation.
How the 24-hour analog dial might be interpreted. Diagram showing how the zodiac is projected on to the ecliptic dial – the symbols are often drawn inside the dial. Stereographic projection from the North Pole. Most astronomical clocks have a 24-hour analog dial around the outside edge, numbered from I to XII then from I to XII again.
Vladimir orbits the Sun in the central main-belt at a distance of 2.6–2.9 AU once every 4 years and 6 months (1,632 days). Its orbit has an eccentricity of 0.06 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Uccle in 1928.
It orbits the Sun in the outer main belt at a distance of 3.4–4.1 AU once every 7 years and 3 months (2,651 days). Its orbit has an eccentricity of 0.09 and an inclination of 10° with respect to the ecliptic. The body's observation arc begins at Heidelberg, two months after its official discovery observation.
50 Aquarii, abbreviated 50 Aqr, is a single star in the zodiac constellation of Aquarius. 50 Aquarii is its Flamsteed designation. It is a faint star with an apparent visual magnitude of 5.76 that is barely visible to the naked eye under good seeing conditions. The star is located near the ecliptic and thus is subject to lunar occultations.
Belopolskya orbits the Sun at a distance of 3.1–3.7 AU once every 6 years and 3 months (2,292 days). Its orbit has an eccentricity of 0.09 and an inclination of 3° with respect to the ecliptic. With these orbital parameters, it belongs to the Cybele asteroids, a dynamical group named after one of the largest asteroids, 65 Cybele.
There is a pronounced mass deficit near the equator at about 90° longitude comparable to Rheasilvia basin on Vesta. There are also two additional smaller (50–70 km in diameter) crater-like depressions near the south pole. Psyche's north pole points towards the ecliptic coordinates , , with a 4° uncertainty. This gives an axial tilt of 95°.
Smaklösa orbits the Sun in the inner main-belt at a distance of 1.7–2.8 AU once every 3 years and 5 months (1,242 days). Its orbit has an eccentricity of 0.23 and an inclination of 7° with respect to the ecliptic. As no precoveries were taken, the asteroid's observation arc begins with its discovery in 1978.
In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue and other sources gave a concurring sidereal period 3.83359 hours, as well as two poles at (46.0°, 10.0°) and (242.0°, 52.0°) in ecliptic coordinates (λ, β) (). Brian Warner also determined two spin axes at (40.0°, 18.0°) and (250.0°, 71.0°) using his data set from 2008 ().
Tau2 Capricorni, Latinized from τ2 Capricorni, is a triple star system in the constellation Capricornus. It is approximately 1,100 light years from Earth based on parallax. The system has a blue-white hue and a combined apparent visual magnitude of +5.20. Because it is positioned near the ecliptic, τ2 Capricorni can be occulted by the Moon.
Its orbit has an eccentricity of 0.19 and an inclination of 4° with respect to the ecliptic. The asteroid was first observed as at Heidelberg Observatory in November 1916. The body's observation arc begins with a precovery taken at the Yerkes Observatory in November 1932, or more than 7 years after its official discovery observation at Simeiz.
Mally orbits the Sun in the central main-belt at a distance of 2.2–3.1 AU once every 4 years and 3 months (1,548 days). Its orbit has an eccentricity of 0.17 and an inclination of 9° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Heidelberg in 1931.
Thomana orbits the Sun in the outer main-belt at a distance of 2.8–3.5 AU once every 5 years and 8 months (2,058 days). Its orbit has an eccentricity of 0.10 and an inclination of 10° with respect to the ecliptic. The asteroid's observation arc begins at Heidelberg, one night after its official discovery observation.
Polonskaya is a member of the Flora family, one of the largest collisional populations of stony asteroids. It orbits the Sun in the inner main-belt at a distance of 1.9–2.8 AU once every 3 years and 6 months (1,295 days). Its orbit has an eccentricity of 0.19 and an inclination of 5° with respect to the ecliptic.
Since Leo begins 120° from the vernal equinox, the longitude in modern form is .; numerous examples of this notation appear throughout the book. In China, ecliptic longitude is measured using 24 Solar terms, each of 15° longitude, and are used by Chinese lunisolar calendars to stay synchronized with the seasons, which is crucial for agrarian societies.
Shanghai is a member of the Themis family, a dynamical family of outer-belt asteroids with nearly coplanar ecliptical orbits. It orbits the Sun at a distance of 2.8–3.6 AU once every 5 years and 7 months (2,047 days). Its orbit has an eccentricity of 0.13 and an inclination of 2° with respect to the ecliptic.
West orbits the Sun in the central main-belt at a distance of 2.4–3.0 AU once every 4 years and 5 months (1,625 days). Its orbit has an eccentricity of 0.12 and an inclination of 6° with respect to the ecliptic. The asteroid observation arc begins at Heidelberg one month after its official discovery observation in March 1938.
Strobel orbits the Sun in the outer main-belt at a distance of 2.8–3.2 AU once every 5 years and 3 months (1,909 days). Its orbit has an eccentricity of 0.07 and an inclination of 19° with respect to the ecliptic. Strobels observation arc begins two nights after its official discovery observation at Heidelberg in 1923.
Ukraina orbits the Sun in the inner main-belt at a distance of 1.9–2.9 AU once every 3 years and 8 months (1,340 days). Its orbit has an eccentricity of 0.21 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins at Heidelberg, five days after its official discovery observation at Simeiz.
The Perseus Family includes several constellations associated with the Perseus myth: Cassiopeia, Cepheus, Andromeda, Perseus, Pegasus, and Cetus (representing the monster sent to devour Andromeda). Menzel also included a few neighboring constellations: Auriga, Lacerta, and Triangulum. Except for Cetus, these constellations all lie north of the ecliptic. The group reaches from near the north celestial pole to declination −30°.
' orbits the Sun at a distance of 6.5–16.7 AU once every 39 years and 7 months (14,460 days; semi- major axis of 11.62 AU). Its orbit has an eccentricity of 0.44 and an inclination of 105° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Siding Spring in December 2008.
19521 Chaos is a cubewano, a Kuiper-belt object not in resonance with any planet. It is a possible dwarf planet, but is likely not a solid body. Chaos was discovered in 1998 by the Deep Ecliptic Survey with Kitt Peak's 4 m telescope. Its albedo is , making it, with its absolute magnitude (H) of 4.8, in diameter.
Venus rotates clockwise, and Uranus has been knocked on its side and rotates almost perpendicular to the rest of the Solar System. The ecliptic remains within 3° of the invariable plane over five million years,Laskar, Jacques (1988), "Secular evolution of the Solar System over 10 million years", Astronomy and astrophysics, no. 198, pp. 341–362 (p.
Leona orbits the Sun in the outer main-belt at a distance of 2.7–4.1 AU once every 6 years and 3 months (2,295 days). Its orbit has an eccentricity of 0.22 and an inclination of 11° with respect to the ecliptic. The asteroid's observation arc begins at the discovering observatory, one night after its official discovery observation.
The S-type asteroid orbits the Sun in the inner main-belt at a distance of 1.8–3.1 AU once every 3 years and 11 months (1,416 days). Its orbit has an eccentricity of 0.25 and an inclination of 7° with respect to the ecliptic. Adalbertas observation arc begins with its official discovery observation at Heidelberg in 1910.
Ecliptic Sagittarius is one of the first recruits in the latest incarnation of the Zodiac. Recruited by their leader Scorpio, Sagittarius was a bow-wielding centaur and has demonstrated a tendency towards violent acts, for which he apparently feels no remorse. He apparently had a relationship with fellow member Pisces. Sagittarius was apparently killed by Weapon X.
Each quadrant of the ecliptic is divided into three equal parts between the four angles. This is the oldest system of quadrant style house division. Although it is attributed to Porphyry of Tyros, this system was first described by the 2nd-century astrologer Vettius Valens, in the 3rd book of his astrological compendium known as The Anthology.
Suttungr is about 7 kilometres in diameter, and orbits Saturn at an average distance of 19,667 Mm in 1029.703 days. It may have formed from debris knocked off Phoebe. The Suttung orbit is retrograde, at an inclination of 174° to the ecliptic (151° to Saturn's equator) and with an eccentricity of 0.131. Its rotation period is hours.
Laurel orbits the Sun in the central main-belt at a distance of 2.4–2.7 AU once every 4 years and 1 month (1,497 days). Its orbit has an eccentricity of 0.07 and an inclination of 14° with respect to the ecliptic. No precoveries were taken and the asteroid's observation arc begins with its discovery observation in 1935.
Its orbit has an eccentricity of 0.12 and an inclination of 6° with respect to the ecliptic. The asteroid was first observed as ' at Uccle Observatory in November 1949. The body's observation arc begins with at precovery taken at Purple Mountain Observatory in October 1973, almost seven years prior to its official discovery observation at La Silla.
Two lightcurves, published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring period of 16.5044 and 16.5045 hours, respectively. Each modeled lightcurve also determined two spin axes of (122.0°, −50.0°) and (301.0°, −59.0°), as well as (282.0°, −79.0°) and (114.0°, −45.0°) in ecliptic coordinates (λ, β), respectively.
Sagan is a member of the Flora family, one of the largest families of stony asteroids. It orbits the Sun in the inner main-belt at a distance of 2.0–2.3 AU once every 3 years and 3 months (1,188 days). Its orbit has an eccentricity of 0.07 and an inclination of 3° with respect to the ecliptic.
Delta Arietis (δ Arietis, abbreviated Delta Ari, δ Ari), officially named Botein , is a star in the northern constellation of Aries, 1.8 degrees north of the ecliptic. The apparent visual magnitude is 4.35, so it is visible to the naked eye. It has an annual parallax shift of 19.22 mas; corresponding to a distance of about from the Sun.
Adelgunde orbits the Sun in the inner main-belt at a distance of 2.0–2.9 AU once every 3 years and 10 months (1,393 days). Its orbit has an eccentricity of 0.19 and an inclination of 7° with respect to the ecliptic. As no precoveries were taken, Adelgundes observation arc begins with its official discovery observation.
Using 638 observations of Comet Coggia made over a period of 185 days, Josef von Hepperger in 1882 calculated an elliptical orbit inclined about 66° to the ecliptic. On 9 July 1874 the comet reached perihelion at about .6758 AU from the Sun. On 23 July the comet made its closest approach to planet Earth at about .
It is possibly a mercury-manganese (HgMn) star, but abundances of other metals are unexpectedly low. Beta Scorpii is 1.01 degree from the ecliptic and can be occulted by the Moon and, very rarely, by planets. On December 9, 1906, it was occulted by Venus. The last occultation by a planet took place on 13 May 1971, by Jupiter.
73-76), which includes the quote about "no serious seventeenth century astronomer" on p. 76; Campbell 1921 (p. 848); Catholic Encyclopedia: Giovanni Battista Riccioli. Within its two volumes were ten "books" covering every subject within astronomy and related to astronomy at the time: #the celestial sphere and subjects such as celestial motions, the equator, ecliptic, zodiac, etc.
The Deep Ecliptic Survey (DES) defines centaurs using a dynamical classification scheme, based on the behavior of orbital integrations over 10 million years. The DES defines centaurs as nonresonant objects whose osculating perihelia are less than the osculating semimajor axis of Neptune at any time during the integration. Using the dynamical definition of a centaur, is a centaur.
Gamma Capricorni (γ Capricorni, abbreviated Gamma Cap, γ Cap), named Nashira , is a giant star in the constellation of Capricornus. Based on parallax measurements obtained during the Hipparcos mission, it is about 139 light- years from the Sun. It is 2.56 degrees south of the ecliptic, so it can be occulted by the Moon, and (rarely) by planets.
' is non-family asteroid of the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.1–3.3 AU once every 4 years and 5 months (1,602 days; semi- major axis of 2.68 AU). Its orbit has an eccentricity of 0.23 and an inclination of 13° with respect to the ecliptic.
In astronomy, an equinox is either of two places on the celestial sphere at which the ecliptic intersects the celestial equator. Although there are two intersections of the ecliptic with the celestial equator, by convention, the equinox associated with the Sun's ascending node is used as the origin of celestial coordinate systems and referred to simply as "the equinox". In contrast to the common usage of spring/vernal and autumnal equinoxes, the celestial coordinate system equinox is a direction in space rather than a moment in time. In a cycle of about 25,700 years, the equinox moves westward with respect to the celestial sphere because of perturbing forces; therefore, in order to define a coordinate system, it is necessary to specify the date for which the equinox is chosen.
Quaoar's minimum orbit intersection distance from Neptune is only 12.3 AU—it does not approach Neptune within this distance over the course of its orbit, as it is not in a mean-motion orbital resonance with Neptune. Simulations by the Deep Ecliptic Survey show that the perihelion and aphelion distances of Quaoar's orbit do not change significantly over the next 10 million years; Quaoar's orbit appears to be stable over the long term. Quaoar is generally classified as a trans-Neptunian object or distant minor planet by the Minor Planet Center since it orbits in the outer Solar System beyond Neptune. Since Quaoar is not in a mean-motion resonance with Neptune, it is also classified as a classical Kuiper belt object (cubewano) by the Minor Planet Center and Deep Ecliptic Survey.
Ixion was discovered with the Víctor M. Blanco Telescope at the Cerro Tololo Observatory Ixion was discovered on 22 May 2001 by a team of American astronomers at the Cerro Tololo Inter-American Observatory in Chile. The discovery formed part of the Deep Ecliptic Survey, a survey conducted by American astronomer Robert Millis to search for Kuiper belt objects located near the ecliptic plane using telescopes at the facilities of the National Optical Astronomy Observatory. On the night of 22 May 2001, American astronomers James Elliot and Lawrence Wasserman identified Ixion in digital images of the southern sky taken with the 4-meter Víctor M. Blanco Telescope at Cerro Tololo. Ixion was first noted by Elliot while compiling two images taken approximately two hours apart, which revealed Ixion's slow motion relative to the background stars.
The north ecliptic pole (Běijí , represented by a red dot which does not correspond to any astral body since the north ecliptic pole is starless, Wújí, "without pole") coiled by Draco (Tiānlóng ), which slithers between the Little Dipper and the Big Dipper (Great Chariot), respectively representing yin and yang, death and life. As the symbol of the "protean" primordial power which contains yin and yang as one, the dragon is the curved line in-between yin and yang in the "diagram of the Supreme Pole" ( Tàijítú, of Tàijí) → 20px. Small seal script form, from the Shuowen Jiezi, of k: qì (pneuma, "breath", "matter–energy", "power" of Heaven). Because all beings are considered coalescences of it, some scholars have employed the term "(poly)pneumatism", first coined by Walter Medhurst (1796–1857), to describe Chinese spirituality.
A 6th century mosaic zodiac wheel in a synagogue, incorporating Greek-Byzantine elements, Beit Alpha, Israel Zodiac circle with planets, c.1000 – NLW MS 735C The division of the ecliptic into the zodiacal signs originates in Babylonian astronomy during the first half of the 1st millennium BC. The zodiac draws on stars in earlier Babylonian star catalogues, such as the MUL.APIN catalogue, which was compiled around 1000 BC. Some constellations can be traced even further back, to Bronze Age (First Babylonian dynasty) sources, including Gemini "The Twins," from MAŠ.TAB.BA.GAL.GAL "The Great Twins," and Cancer "The Crab," from AL.LUL "The Crayfish," among others. Around the end of the 5th century BC, Babylonian astronomers divided the ecliptic into 12 equal "signs", by analogy to 12 schematic months of 30 days each.
Delta Cancri (δ Cancri, abbreviated Delta Cnc, δ Cnc) is a double star about 180 light-years from the Sun in the constellation of Cancer. Its two main constituents are designated Delta Cancri A and B. A is itself a binary star whose components are Delta Cancri Aa (formally named Asellus Australis , the traditional name of the entire system) and Ab. The star system is 0.08 degree north of the ecliptic, so it can be occulted by the Moon and more rarely by planets; it is occulted (eclipsed) by the sun from about 31 July to 2 August.In the Sky Earth astronomy reference utility showing the ecliptic and relevant date as at J2000 - present Thus the star can be viewed the whole night, crossing the sky at the start of February.
Ultimately, Between the Buried & Me, despite employing many tropes and influences, come off sounding like no one but themselves." Calum Slingerland of Exclaim! opined, "While the noticeable shift away from death metal may discourage some, Coma Ecliptic succeeds in pushing Between the Buried and Me's creativity in a new direction, avoiding a simple rehash of their winning formula." Dom Lawson from The Guardian gave the album a perfect rating calling it "ingenious, sprawling prog-metal" and saying "From the rock opera crescendos of the opening "Node" onwards, the album dares to be both a quintessentially prog-rock experience and a timely act of modern metal derring-do." Chris Cope of Prog added that "at its best, Coma Ecliptic holds some of this band’s most impressive moments to date.
Her two first EPs Let's Run Wild and Born to Fly were released via UK label This Is Music Ltd in 2012. The songs on Let's Run Wild were co-written and co-produced by Findlay Brown. Her debut album, Ecliptic, was independently released in 2015. The album accrued radio spins from over 50 stations nationwide including Los Angeles' KCRW.
The spacecraft spin axis was normal to the ecliptic plane, and the spin rate was 22.3 rpm. The data telemetry rate was 1600 bps. The spacecraft was in the solar wind for 7 to 8 days of every 12 days orbit. Telemetry coverage was 90% in the early years, but only 60-70% through most of the 1980s and early 1990s.
Leontina is an X-type asteroid in the SMASS classification. It orbits the Sun at a distance of 3.0–3.4 AU once every 5 years and 9 months (2,097 days). Its orbit is tilted by 9 degrees to the plane of the ecliptic and shows an eccentricity of 0.07. Multiple lightcurve analysis rendered a well-defined, concurring rotation period of 6.79 hours.
In such cases, international collaborations are highly useful with each observatory covering a different section of the lightcurve. In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from a large collaboration of individual observers (such as above). The study also determined two spin axes of (344.0°, 27.0°) and (164.0°, 8.0°) in ecliptic coordinates (λ, β).
Since 1997, a large number of rotational lightcurves of Gretia have been obtained from photometric observations. Analysis of the best- rated lightcurves gave a rotation period of 5.778 hours with a maximal brightness amplitude from 0.26 to 0.75 magnitude (). The asteroid's spin axis of (92.0°, 67.0°) and (247.0°, 48.0°) in ecliptic coordinates (λ, β) have also been derived from modeled lightcurves ().
Because the obliquity of the ecliptic is slowly decreasing, the values during the lives of Jaghmini and al-Tusi's differ from modern values. As of 2000, the appropriate solar positions are 6°40′ Gemini and 23°20′ Cancer. Other than specifying the sun's position, the passage by al-Tusi describes how to convert the noontime in Mecca to the local time.
IMAP-Lo is a single-pixel neutral atom imager that gives energy and angle-resolved measurements of ISN atoms (H, He, O, Ne, and D) tracked over >180° in ecliptic longitude and energy resolved global maps of ENA H and O. IMAP-Lo has heritage from the IBEX-Lo on Interstellar Boundary Explorer (IBEX) but provides much larger collection power.
Manwë was discovered on 25 August 2003 by M. W. Buie at Cerro Tololo as a part of the Deep Ecliptic Survey. The object was named after Manwë, the fictional king of the Valar in J. R. R. Tolkien's Middle-earth legendarium. Manwë is foremost among the great spirits who rule the world. Manwë takes special responsibility for the air and winds.
Xanthippe is a non-family asteroid from the main belt's background population. It orbits the Sun in the central main-belt at a distance of 2.1–3.3 AU once every 4 years and 6 months (1,645 days; semi-major axis of 2.73 AU). Its orbit has an eccentricity of 0.23 and an inclination of 10° with respect to the ecliptic.
The ecliptic concrete structure is high, with length on bottom and on top and its watershed is long.Amirkabir Dam Inaugurated The average annual water inflow to its reservoir is 472 million cubic meters. The total capacity of the dam's reservoir is 202 million cubic meters. The bottom elevation of reservoir and normal water surface elevation of reservoir are and respectively.
Centaurs have short dynamical lives due to strong interactions with the giant planets. Okyrhoe is estimated to have an orbital half-life of about 670 kiloannum. Of objects listed as a centaur by the Minor Planet Center (MPC), JPL, and the Deep Ecliptic Survey (DES), Okyrhoe has the second smallest perihelion distance of a numbered centaur. Numbered centaur has a smaller perihelion distance.
Bacchus orbits the Sun at a distance of 0.7–1.5 AU once every 1 years and 1 month (409 days). Its orbit has an eccentricity of 0.35 and an inclination of 9° with respect to the ecliptic. The asteroid's observation arc begins with its official discovery observation at Palomar. Due to its eccentric orbit, it is also a Venus-crosser.
Kanagawa orbits the Sun in the outer main-belt at a distance of 2.5–3.5 AU once every 5 years and 2 months (1,882 days). Its orbit has an eccentricity of 0.16 and an inclination of 18° with respect to the ecliptic. No precoveries were taken prior to its discovery. The asteroid's observation arc begins with its official discovery observation at Hadano.
Inari is a member the Eos family (), one of the asteroid belt's largest families with nearly 10,000 known asteroids. It orbits the Sun in the outer main belt at a distance of 2.8–3.2 AU once every 5 years and 3 months (1,903 days). Its orbit has an eccentricity of 0.05 and an inclination of 9° with respect to the ecliptic.
The S-type asteroid is a member of the Eos family. It orbits the Sun in the outer main-belt at a distance of 2.7–3.3 AU once every 5 years and 3 months (1,911 days). Its orbit has an eccentricity of 0.11 and an inclination of 11° with respect to the ecliptic. Heike was first identified as at Heidelberg Observatory in 1906.
Gaby orbits the Sun at a distance of 1.9–2.9 AU once every 3 years and 9 months (1,370 days). Its orbit has an eccentricity of 0.21 and an inclination of 11° with respect to the ecliptic. No precoveries were taken, and no prior identifications were made of Gaby. The body's observation arc begins 2 months after its official discovery observation at Heidelberg.
The C-type asteroid orbits the Sun at a distance of 2.3–4.0 AU once every 5 years and 8 months (2,063 days). Its orbit has an eccentricity of 0.28 and an inclination of 1° with respect to the ecliptic. Gezelles first identification as at Heidelberg Observatory remained unused. Its observation arc begins 9 days after its official discovery observation.
Guo Shou-Jing orbits the Sun at a distance of 1.9–2.7 AU once every 3 years and 7 months (1,298 days). Its orbit has an eccentricity of 0.18 and an inclination of 3° with respect to the ecliptic. The body's observation arc begins 11 years prior to its official discovery observation, with a precovery taken at Palomar Observatory in August 1953.
The S-type asteroid orbits the Sun at a distance of 1.7–2.9 AU once every 3 years and 6 months (1,292 days). Its orbit has an eccentricity of 0.27 and an inclination of 8° with respect to the ecliptic. Gothards observation arc begins 14 years after its official discovery observation, when it was identified as at Uccle Observatory in 1955.
Gordonmoore orbits the Sun at a distance of 1.3–3.1 AU once every 3 years and 3 months (1,192 days). Its orbit has an eccentricity of 0.43 and an inclination of 8° with respect to the ecliptic. It has a minimum orbit intersection distance with Earth of , or 96.3 lunar distance. Due to its eccentric orbit, Gordonmoore is also Mars-crosser.
Ebella orbits the Sun in the central main-belt at a distance of 1.8–3.2 AU once every 4.04 years (1,474 days). Its orbit has an eccentricity of 0.27 and an inclination of 9° with respect to the ecliptic. As no precoveries were taken and no prior identifications were made, the asteroid's observation arc begins at Heidelberg with its official discovery observation.
The S-type asteroid is a member of the Koronis family, a group consisting of about 200 known bodies. It orbits the Sun in the outer main-belt at a distance of 2.6–3.2 AU once every 4 years and 11 months (1,810 days). Its orbit has an eccentricity of 0.09 and an inclination of 3° with respect to the ecliptic.
Akka orbits the Sun at a distance of 1.1–2.6 AU once every 2 years and 6 months (904 days). Its orbit has an eccentricity of 0.41 and an inclination of 2° with respect to the ecliptic. The first observation was made at Siding Spring Observatory in May 1992, extending the asteroid's observation arc by just two weeks prior to its discovery.
Aktsynovia is a non-family asteroid from the main belt's background population. It orbits the Sun in the inner asteroid belt at a distance of 2.1–2.7 AU once every 3 years and 8 months (1,349 days). Its orbit has an eccentricity of 0.13 and an inclination of 4° with respect to the ecliptic. No precovery was ever taken for this asteroid.
Altdorfer is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbits the Sun in the inner main-belt at a distance of 2.0–2.5 AU once every 3 years and 4 months (1,223 days). Its orbit has an eccentricity of 0.10 and an inclination of 3° with respect to the ecliptic.
Broederstroom is a member of the Flora family. It orbits the Sun in the inner main-belt at a distance of 1.9–2.6 AU once every 3 years and 4 months (1,229 days). Its orbit has an eccentricity of 0.15 and an inclination of 2° with respect to the ecliptic. No precoveries were taken, and no prior identifications were made.
Bruce Helin is a member of the Phocaea family (). It orbits the Sun in the inner main-belt at a distance of 1.9–2.9 AU once every 3 years and 8 months (1,326 days). Its orbit has an eccentricity of 0.21 and an inclination of 23° with respect to the ecliptic. It was first observed at at Heidelberg Observatory in 1908.
Porvoo orbits the Sun in the inner main-belt at a distance of 2.1–2.6 AU once every 3 years and 7 months (1,317 days). Its orbit has an eccentricity of 0.13 and an inclination of 4° with respect to the ecliptic. As no precoveries were taken, and no prior identifications were made, Porvoos observation arc begins with its official discovery observation.
Poseidon orbits the Sun at a distance of 0.6–3.1 AU once every 2 years and 6 months (908 days). Its orbit has an eccentricity of 0.68 and an inclination of 12° with respect to the ecliptic. As no precoveries were taken, the asteroid's observation arc begins with its discovery in 1987. Poseidon may be associated with the Taurid Complex of meteor showers.
Katyusha is a member of the Flora family, one of the largest groups of stony asteroids in the inner main- belt. It orbits the Sun in the inner main-belt at a distance of 1.9–2.5 AU once every 3 years and 3 months (1,200 days). Its orbit has an eccentricity of 0.13 and an inclination of 7° with respect to the ecliptic.
It is a member of the Flora family, one of the largest families of stony asteroids in the asteroid belt. It orbits the Sun in the inner main-belt at a distance of 2.0–2.5 AU once every 3 years and 5 months (1,233 days). Its orbit has an eccentricity of 0.13 and an inclination of 4° with respect to the ecliptic.
Kozai orbits the Sun in the inner main-belt at a distance of 1.5–2.2 AU once every 2 years and 6 months (912 days). Its orbit has an eccentricity of 0.20 and an inclination of 47° with respect to the ecliptic. On 10 January 2044, the asteroid will make a close approach to Mars, passing the Red Planet at a distance of .
Knushevia is a bright member of the Hungaria family, which forms the innermost dense concentration of asteroids in the Solar System. It orbits the Sun in the inner main-belt at a distance of 1.8–2.1 AU once every 2 years and 9 months (1,003 days). Its orbit has an eccentricity of 0.07 and an inclination of 22° with respect to the ecliptic.
It is estimated that the family is million years old. It orbits the Sun in the at a distance of 2.5–3.9 AU once every 5 years and 8 months (2,064 days). Its orbit has an eccentricity of 0.22 and an inclination of 9° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Nankin in 1964.
Leakey is a member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System. It orbits the Sun in the inner main-belt at a distance of 1.7–2.0 AU once every 2 years and 7 months (939 days). Its orbit has an eccentricity of 0.08 and an inclination of 22° with respect to the ecliptic.
Mombasa orbits the Sun at a distance of 2.4–3.2 AU once every 4 years and 9 months (1,720 days). Its orbit has an eccentricity of 0.14 and an inclination of 17° with respect to the ecliptic. Mombasa was first identified as at Lowell Observatory, extending the body's observation arc by 4 years prior to its official discovery at Johannesburg.
In 2004, a rotational lightcurve of Royer was obtained from photometric observations by Brazilian and Argentine astronomers. Lightcurve analysis gave a rotation period of 3.866 hours with a brightness amplitude of 0.44 magnitude (). In 2016, a modeled lightcurves using photometric data from various sources, rendered a sidereal period of 3.88494 and two spin axes of (258.0°, 74.0°) and (54.0°, 37.0°) in ecliptic coordinates.
' is a classical trans-Neptunian object and member of Haumea family from the Kuiper belt located in the outermost regions of the Solar System, approximately 300 kilometers in diameter. It was first observed on 23 September 2003, by astronomers of the Canada–France Ecliptic Plane Survey at Mauna Kea Observatories on Hawaii. The surface of is made of water ice.
Camoes orbits the Sun in the inner main-belt at a distance of 2.2–2.6 AU once every 3 years and 9 months (1,359 days). Its orbit has an eccentricity of 0.07 and an inclination of 8° with respect to the ecliptic. The asteroid's observation arc starts in 1979, as no precoveries were taken and no identifications were made prior to its discovery.
74 Virginis is a single star in the zodiac constellation of Virgo. It is visible to the naked eye as a faint red-hued star with an apparent visual magnitude of 4.69. The star is positioned near the ecliptic and thus is subject to lunar occultations. The measured annual parallax of provides a distance estimate of around 400 light years from the Sun.
The orbit of compared to Pluto and Neptune has a semi- major axis (average distance from the Sun) near the edge of the classical belt. The Deep Ecliptic Survey (DES) list this trans-Neptunian object as a twotino that stays in a 1:2 orbital resonance with the planet Neptune (for every one orbit that a twotino makes, Neptune orbits twice).
The S-type asteroid is a member of the Phocaea family (), a group of asteroids with similar orbital characteristics. It orbits the Sun in the inner main-belt at a distance of 1.7–2.8 AU once every 3 years and 5 months (1,248 days). Its orbit has an eccentricity of 0.24 and an inclination of 23° with respect to the ecliptic.
It orbits the Sun at a distance of 4.7–5.9 AU once every 12 years and 3 months (4,459 days; semi-major axis of 5.3 AU). Its orbit has an eccentricity of 0.11 and an inclination of 18° with respect to the ecliptic. The body's observation arc begins at Heidelberg 6 days after its official discovery observations in August 1936.
Rantaseppä is a member of the Flora family of stony asteroids, one of the largest families of the main belt. It orbits the Sun in the inner main-belt at a distance of 1.8–2.7 AU once every 3 years and 4 months (1,231 days). Its orbit has an eccentricity of 0.20 and an inclination of 4° with respect to the ecliptic.
Vinterhansenia is classified as both C-type and X-type asteroid. It orbits the Sun in the inner main-belt at a distance of 2.1–2.6 AU once every 3 years and 8 months (1,335 days). Its orbit has an eccentricity of 0.11 and an inclination of 3° with respect to the ecliptic. Vinterhansenia was first identified as at Heidelberg Observatory in 1906.
This C-type asteroid orbits the Sun at a distance of 2.8–3.5 AU once every 5 years and 7 months (2,045 days). Its orbit has an eccentricity of 0.10 and an inclination of 10° with respect to the ecliptic. Volodias observation arc begins with its official discovery at Johannesburg, as no precoveries were taken, and no prior identifications were made.
2018 BD is an Apollo asteroid. It orbits the Sun at a distance of 0.75–1.36 AU once every 13 months (395 days; semi-major axis of 1.05 AU). Its orbit has an eccentricity of 0.29 and an inclination of 2° with respect to the ecliptic. The object has an exceptionally low minimum orbital intersection distance with Earth of , or 0.002 lunar distances.
Marlene is not a member of any known asteroid family. It orbits the Sun in the outer main-belt at a distance of 2.6–3.2 AU once every 5.02 years (1,832 days). Its orbit has an eccentricity of 0.10 and an inclination of 4° with respect to the ecliptic. The asteroid was first identified as at the discovering observatory in October 1903.
Stroobantia orbits the Sun at a distance of 2.8–3.0 AU once every 5.01 years (1,829 days). Its orbit has an eccentricity of 0.03 and an inclination of 8° with respect to the ecliptic. First identified as at Heidelberg in 1926, the asteroid's observation arc begins at Algiers Observatory in 1931, or three years after its official discovery observation at Uccle.
Jérôme orbits the Sun in the middle main-belt at a distance of 2.3–3.2 AU once every 4 years and 8 months (1,697 days). Its orbit has an eccentricity of 0.16 and an inclination of 9° with respect to the ecliptic. The body's observation arc starts with its official discovery observation, as no precoveries were taken and no prior identifications were made.
Arago orbits the Sun in the outer main-belt at a distance of 2.8–3.5 AU once every 5 years and 8 months (2,058 days). Its orbit has an eccentricity of 0.12 and an inclination of 19° with respect to the ecliptic. The asteroid's observation arc begins at Uccle Observatory in 1935, twelve years after its official discovery observation at Simeiz.
Euler is a non- family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun at a distance of 2.3–2.6 AU once every 3 years and 9 months (1,373 days). Its orbit has an eccentricity of 0.07 and an inclination of 9° with respect to the ecliptic.
The asteroid orbits the Sun at a distance of 1.2–3.1 AU once every 3 years and 2 months (1,147 days). Its orbit has an eccentricity of 0.44 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with its first observation at the Siding Spring Observatory, five months prior to its official discovery observation at Kushiro.
The most detailed analysis indicates that it points either towards about ecliptic coordinates (β, λ) = (70°, 55°) or (40°, 255°) with a 10° uncertainty. This gives an axial tilt of about 14° or 54°, respectively. In 1988 a search for satellites or dust orbiting this asteroid was performed using the UH88 telescope at the Mauna Kea Observatories, but the effort came up empty.
It is convenient to define the orientation of an ECI frame using the Earth's orbit plane and the orientation of the Earth's rotational axis in space.David A. Vallado and Wayne D. McClain, "Fundamentals of Astrodynamics and Applications," 3rd ed. Microcosm Press, 2007, pp. 153–162. The Earth's orbit plane is called the ecliptic, and it does not coincide with the Earth's equatorial plane.
In 1986, several rotational lightcurves of Tombecka were obtained from photometric observations. Lightcurve analysis gave a rotation period between 6.0 and 6.0508 hours with a brightness variation of 0.35 to 0.50 magnitude (). In 2006, an international study modeled a lightcurve with a concurring period of 6.05017 hours and determined a spin axis of (4.0°, 62.0°) in ecliptic coordinates (λ, β) ().
Sonneberga orbits the Sun in the central main-belt at a distance of 2.5–2.8 AU once every 4 years and 5 months (1,603 days). Its orbit has an eccentricity of 0.06 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins with its official discovery observation, as no precoveries were taken, and no prior identifications were made.
Beate orbits the Sun in the outer main-belt at a distance of 3.0–3.2 AU once every 5 years and 5 months (1,990 days). Its orbit has an eccentricity of 0.04 and an inclination of 9° with respect to the ecliptic. The asteroid's observation arc begins at the discovering observatory in May 1925, 3 weeks after its official discovery observation.
Richilde is a non-family asteroid from the main-belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.4–3.0 AU once every 4 years and 6 months (1,629 days; semi-major axis of 2.71 AU). Its orbit has an eccentricity of 0.12 and an inclination of 10° with respect to the ecliptic.
In the Almagest, Ptolemy describes a meridian circle which consisted of a fixed graduated outer ring and a movable inner ring with tabs that used a shadow to set the Sun's position. It was mounted vertically and aligned with the meridian. The instrument was used to measure the altitude of the Sun at noon in order to determine the path of the ecliptic.
Observers on other worlds would, of course, see objects in that sky under much the same conditions – as if projected onto a dome. Coordinate systems based on the sky of that world could be constructed. These could be based on the equivalent "ecliptic", poles and equator, although the reasons for building a system that way are as much historic as technical.
Tau2 Aquarii (τ2 Aqr, τ2 Aquarii) is the Bayer designation for a star in the equatorial constellation of Aquarius. It is visible to the naked eye with an apparent visual magnitude of +4.0. Because the star lies near the ecliptic it is subject to occultations by the Moon. This is an orange-hued giant star with a stellar classification of K5 III.
Clifford is a member of the group of main-belt asteroids known as Mars-crosser asteroids, specifically, it is listed as an Outer- grazer. It orbits the Sun at a distance of 1.6–2.4 AU once every 2 years and 10 months (1,040 days). Its orbit has an eccentricity of 0.20 and an inclination of 21° with respect to the ecliptic.
Sampo is a member of the Eos family (), the largest asteroid family in the outer main belt consisting of nearly 10,000 asteroids. It orbits the Sun in at a distance of 2.8–3.2 AU once every 5 years and 3 months (1,911 days). Its orbit has an eccentricity of 0.06 and an inclination of 11° with respect to the ecliptic.
Sendai is a member of the Flora family, one of the largest groups of stony asteroids in the main- belt. It orbits the Sun in the inner main-belt at a distance of 1.8–2.5 AU once every 3 years and 3 months (1,176 days). Its orbit has an eccentricity of 0.16 and an inclination of 7° with respect to the ecliptic.
Seneca orbits the Sun at a distance of 1.1–4.0 AU once every 3 years and 12 months (1,457 days). Its orbit has an eccentricity of 0.57 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins with its official discovery observation in 1978, as no precoveries were taken, and no prior identifications were made.
Sersic is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbits the Sun in the inner main-belt at a distance of 2.0–2.5 AU once every 3 years and 4 months (1,228 days). Its orbit has an eccentricity of 0.11 and an inclination of 4° with respect to the ecliptic.
Sevastopol is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbits the Sun in the inner main-belt at a distance of 1.8–2.6 AU once every 3 years and 3 months (1,179 days). Its orbit has an eccentricity of 0.18 and an inclination of 4° with respect to the ecliptic.
Carla orbits the Sun at a distance of 2.9–3.4 AU once every 5 years and 7 months (2,051 days). Its orbit has an eccentricity of 0.07 and an inclination of 3° with respect to the ecliptic. It was first identified as at Heidelberg 1930. The body's observation arc, however, begins the night prior to its official discovery observation in 1938.
The fictional Ern Malley achieved a measure of celebrity. The poems are regularly re-published and quoted. There have been at least 20 publications of the Darkening Ecliptic, either complete or partial. It has reappeared – not only in Australia, but in London, Paris, Lyons, Kyoto, New York and Los Angeles – with a regularity that would be the envy of any real Australian poet.
The Sun moved at an oblique angle to the circles, which obliquity brought it now to the north, now to the south. The circle of the Sun was the ecliptic. It was the center of a band called the zodiac on which various constellations were located. The shadow cast by a vertical rod at noon was the basis for defining zonation.
The S-type asteroid orbits the Sun in the inner main-belt at a distance of 2.0–2.4 AU once every 3 years and 4 months (1,210 days). Its orbit has an eccentricity of 0.09 and an inclination of 1° with respect to the ecliptic. No precoveries were taken. The asteroid's observation arc begins 3 days after its official discovery observation.
Wright orbits the Sun at a distance of 1.5–1.9 AU once every 2 years and 3 months (816 days). Its orbit has an eccentricity of 0.11 and an inclination of 21° with respect to the ecliptic. As no precoveries were taken and no previous identifications were made, Wright's observation arc begins with its official discovery observation at Mount Hamilton in 1947.
The S-type asteroid orbits the Sun at a distance of 1.9–3.2 AU once every 4 years and 2 months (1,507 days). Its orbit has an eccentricity of 0.26 and an inclination of 13° with respect to the ecliptic. Xosas observation arc begins with its official discovery observation, as no precoveries were taken and no prior identifications were made.
Walraven is a stony S-type asteroid that orbits the Sun in the inner main-belt at a distance of 1.8–2.8 AU once every 3 years and 6 months (1,270 days). Its orbit has an eccentricity of 0.23 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins one day prior to its official discovery observation.
Subbotina is a non- family asteroid from the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.4–3.2 AU once every 4 years and 8 months (1,700 days; semi-major axis of 2.79 AU). Its orbit has an eccentricity of 0.14 and an inclination of 2° with respect to the ecliptic.
Suruga is an orbital member of the Vesta family in the inner main-belt. It orbits the Sun at a distance of 2.3–2.6 AU once every 3 years and 9 months (1,380 days). Its orbit has an eccentricity of 0.06 and an inclination of 7° with respect to the ecliptic. The asteroid was first identified as at Crimea–Nauchnij in 1979.
Suvanto is a member of the Eunomia family, the most prominent family in the intermediate main-belt, which mostly consists of stony S-type asteroids. It orbits the Sun at a distance of 2.3–3.0 AU once every 4 years and 4 months (1,577 days). Its orbit has an eccentricity of 0.15 and an inclination of 13° with respect to the ecliptic.
Union is not a member of any known asteroid family. It orbits the Sun in the outer main belt at a distance of 2.0–3.8 AU once every 5.01 years (1,830 days). Its orbit has an eccentricity of 0.31 and an inclination of 26° with respect to the ecliptic. In 1929, the asteroid was first identified as at the Uccle Observatory in Belgium.
Tokai is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbits the Sun in the inner main-belt at a distance of 2.1–2.4 AU once every 3 years and 4 months (1,213 days). Its orbit has an eccentricity of 0.07 and an inclination of 4° with respect to the ecliptic.
It orbits the Sun at a distance of 0.3–0.8 AU once every 5 months (151 days; semi-major axis of 0.56 AU). Its orbit has an eccentricity of 0.43 and an unusually high inclination of 30° with respect to the ecliptic. The asteroids and are the only known asteroids with closer aphelions. The orbital evolution of is similar to that of .
It is located near the ecliptic and thus is subject to lunar occultations. The cluster is located 2,050 light years away. Estimates for the number of cluster members range from 169 up to 414, with a directly-counted mass of ; by application of the virial theorem. The cluster is around 330 million years old with a near-solar metallicity of [Fe/H] = −0.04.
242 Detailed records of astronomical observations began during the Warring States period (fourth century BCE) and flourished from the Han period onward. Chinese astronomy was equatorial, centered as it was on close observation of circumpolar stars, and was based on different principles from those prevailing in traditional Western astronomy, where heliacal risings and settings of zodiac constellations formed the basic ecliptic framework.
Aquitania is the largest member of the Postrema family (), a mid-sized central asteroid family of little more than 100 members. It orbits the Sun in the central main-belt at a distance of 2.1–3.4 AU once every 4 years and 6 months (1,657 days). Its orbit has an eccentricity of 0.24 and an inclination of 18° with respect to the ecliptic.
Ecliptic Leo was a later addition to the Zodiac who resembled a humanoid lion. As mean, nasty, and brutal as the other Zodiac man-animals, Leo was also a boastful braggart, openly talking of the group’s plans. He accompanied Capricorn and Aries in the theft of Department H's super-organism. He was later killed with the rest of the Zodiac by Weapon X.
Ho, Peng Yoke. (2000). Li, Qi, and Shu: An Introduction to Science and Civilization in China, p. 105. Mineola: Dover Publications. . These possible influences include a pseudo-geometrical method for converting between equatorial and ecliptic coordinates, the systematic use of decimals in the underlying parameters, and the application of cubic interpolation in the calculation of the irregularity in the planetary motions.
It orbits the Sun at a distance of 3.6–12.8 AU once every 23 years and 4 months (8,520 days; semi-major axis of 8.16 AU). Its orbit has an eccentricity of 0.57 and an inclination of 79° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at the Siding Spring Observatory in December 2004.
Breviceps bagginsi is a mycrohylid (narrow-mouthed) frog from the family of Brevicipitidae discovered in the year 2003. The body size of male individuals varies from 20–25.9 mm and females measure approximately 28.7 mm in length. With its highly truncated snout it is well adapted to its burrowing lifestyle. They have a characteristic tympanic membrane and their pupil is horizontally ecliptic.
The inclination of Earth's orbit drifts up and down relative to its present orbit. This three-dimensional movement is known as "precession of the ecliptic" or "planetary precession". Earth's current inclination relative to the invariable plane (the plane that represents the angular momentum of the Solar System, approximately the orbital plane of Jupiter) is 1.57°. Milankovitch did not study planetary precession.
The orbit of Chaos (white) compared Pluto and the four giant planets: Jupiter, Saturn, Uranus, and Neptune with positions for 2019 19521 Chaos has an orbital period of approximately 309 years. Its orbit is longer, but less eccentric than the orbit of Pluto. 19521 Chaos's orbit is inclined approximately 12° to the ecliptic. Its orbit never crosses the orbit of Neptune.
Computer simulations have shown that the Pleiades were probably formed from a compact configuration that resembled the Orion Nebula. Astronomers estimate that the cluster will survive for about another 250 million years, after which it will disperse due to gravitational interactions with its galactic neighborhood. Together with the open star cluster of the Hyades the Pleiades form the Golden Gate of the Ecliptic.
53311 Deucalion , provisional designation , is a trans-Neptunian object from the classical Kuiper belt, located in the outermost region of the Solar System, approximately . The cubewano belongs to the cold population and was discovered on 18 April 1999, by the Deep Ecliptic Survey at the Kitt Peak National Observatory in Arizona, United States. It was named after Deucalion, from Greek mythology.
McAuliffe orbits the Sun at a distance of 1.2–2.6 AU once every 2 years and 7 months (941 days). Its orbit has an eccentricity of 0.37 and an inclination of 5° with respect to the ecliptic. It has an Earth minimum orbital intersection distance of , which translates into 79.5 lunar distances. Due to its eccentric orbit, McAuliffe is also a Mars-crosser.
Jade dragon of the Hongshan culture. The dragon, associated to the constellation Draco winding the north ecliptic pole, represents the "protean" primordial power, which embodies yin and yang in unity. dǐng (ritual cauldron) with tāotiè motif. According to Didier, both the cauldrons and the taotie symmetrical faces originate as symbols of Di as the squared north celestial pole, with four faces.
Catriona is not a member of any identified asteroid family. It orbits the Sun in the outer main belt at a distance of 2.3–3.6 AU once every 5.00 years (1,826 days). Its orbit has an eccentricity of 0.23 and an inclination of 17° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Johannesburg.
The South Ecliptic pole also lies within this constellation. Even though the name Dorado is not Latin but Portuguese, astronomers give it the Latin genitive form Doradus when naming its stars; it is treated (like the adjacent asterism Argo Navis) as a feminine proper name of Greek origin ending in -ō (like Io or Callisto or Argo), which have a genitive ending -ūs.
Ecliptic Virgo is one of the first recruits in the latest incarnation of the Zodiac. She was quiet and loyal to Scorpio, who was in love with her. She came to like Paris during her time stranded there without her teleportation device, but it is unknown if it was she or Taurus who killed her "rescuers." Virgo was apparently killed by Weapon X.
Lightcurve-based 3D-model of Hebe Size comparison: the first 10 asteroids profiled against the Moon. Hebe is sixth from the left. Lightcurve analysis suggests that Hebe has a rather angular shape, which may be due to several large impact craters. Hebe rotates in a prograde direction, with the north pole pointing towards ecliptic coordinates (β, λ) = (45°, 339°) with a 10° uncertainty.
Esclangona is a member of the Hungaria family, which form the innermost concentration of asteroids in the Solar System. It orbits the Sun in the inner main-belt at a distance of 1.8–1.9 AU once every 2 years and 7 months (931 days). Its orbit has an eccentricity of 0.03 and an inclination of 22° with respect to the ecliptic.
Mündleria orbits the Sun in the inner main-belt at a distance of 2.0–2.7 AU once every 3 years and 8 months (1,339 days). Its orbit has an eccentricity of 0.16 and an inclination of 13° with respect to the ecliptic. Mündlerias observation arc begins with its official discovery observation in 1938. It was first identified as at Heidelberg in 1923.
Bulgaria is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbits the Sun in the inner main-belt at a distance of 2.0–2.5 AU once every 3 years and 4 months (1,225 days). Its orbit has an eccentricity of 0.12 and an inclination of 5° with respect to the ecliptic.
Cora orbits the Sun in the middle main-belt at a distance of 2.1–3.3 AU once every 4 years and 6 months (1,640 days). Its orbit has an eccentricity of 0.22 and an inclination of 13° with respect to the ecliptic. The body's observation arc begins 4 years after its discovery with the first used observation made at Heidelberg in 1906.
Edith orbits the Sun in the outer main-belt at a distance of 2.6–3.7 AU once every 5 years and 7 months (2,050 days). Its orbit has an eccentricity of 0.18 and an inclination of 3° with respect to the ecliptic. The body's observation arc begins at Heidelberg, five days after its official discovery observation (first recorded observation at the MPC).
Tergeste orbits the Sun in the outer main-belt at a distance of 2.8–3.3 AU once every 5 years and 3 months (1,915 days). Its orbit has an eccentricity of 0.08 and an inclination of 13° with respect to the ecliptic. The body's observation arc begins with its first used observation at Koenigsberg Observatory, 2 days after its official discovery at Heidelberg.
Orbital diagram of Icarus Icarus orbits the Sun at a distance of 0.2–2.0 AU once every 13 months (409 days). Its orbit has an eccentricity of 0.83 and an inclination of 23° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Palomar. At perihelion, Icarus comes closer to the Sun than Mercury, i.e.
Tolkien is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbits the Sun in the inner main-belt at a distance of 2.0–2.4 AU once every 3 years and 3 months (1,202 days). Its orbit has an eccentricity of 0.10 and an inclination of 3° with respect to the ecliptic.
Amenemhêt orbits the Sun in the central main-belt at a distance of 2.2–3.3 AU once every 4 years and 6 months (1,633 days). Its orbit has an eccentricity of 0.20 and an inclination of 15° with respect to the ecliptic. Its observation arc already begins in 1955, due to precoveries taken at the U.S. Goethe Link Observatory in Indiana.
Many astronomers failed to find any moon during their observations of Venus, including William Herschel in 1768. Cassini originally observed Neith to be one-fourth the diameter of Venus. In 1761, Lagrange announced that Neith's orbital plane was perpendicular to the ecliptic. In 1766, the director of the Vienna Observatory speculated that the observations of the moon were optical illusions.
Belisana is a non-family asteroid from the main belt's background population. It orbits the Sun in the inner main-belt at a distance of 2.4–2.6 AU once every 3 years and 10 months (1,409 days; semi-major axis of 2.46 AU). Its orbit has an eccentricity of 0.04 and an inclination of 2° with respect to the ecliptic.
Istria is a non-family asteroid from the main belt's background population. It orbits the Sun in the central main- belt at a distance of 1.8–3.8 AU once every 4 years and 8 months (1,703 days; semi-major axis of 2.79 AU). Its orbit has an eccentricity of 0.35 and an inclination of 26° with respect to the ecliptic.
' orbits the Sun at a distance of 16.8–538.9 AU once every 4631 years and 1 month (1,691,491 days; semi-major axis of 277.83 AU). Its orbit has an eccentricity of 0.94 and an inclination of 85° with respect to the ecliptic. The body's observation arc begins with its official discovery observation by Pan-STARRS at Haleakala Observatory in May 2013.
2019 was predicted to be the closest post-perihelion encounter with Earth since 1975. The Taurid swarm was expected to pass below the ecliptic between June 23 – July 17. During 2019 astronomers searched for hypothesized asteroids ~100 meters in diameter from the Taurid swarm between July 5–11, and July 21 – August 10. There were no reports of discoveries of any such objects.
Aten orbits the Sun at a distance of 0.8–1.1 AU once every 11 months (347 days). Its orbit has an eccentricity of 0.18 and an inclination of 19° with respect to the ecliptic. A first precovery was taken at the discovering observatory in December 1955, extending the body's observation arc by more than 20 years prior to its official discovery observation.
Computation of dodecatemoria could have helped the ancient astronomer by, simply, giving him more symbolic data to interpret. The dodecatemoria could also crudely represent the motion of the moon across the ecliptic during the course of one month. Possibly they use a "virtual moon", imagined conjunct with the Sun (i.e., new) at the beginning of a sign, to symbolize divisions within the sign.
Balam is a member of the Flora family, a very large group of stony asteroids in the inner main-belt. It orbits the Sun in the inner main-belt at a distance of 2.0–2.5 AU once every 3 years and 4 months (1,222 days). Its orbit has an eccentricity of 0.11 and an inclination of 5° with respect to the ecliptic.
Virgo is one of the constellations of the zodiac. Its name is Latin for virgin, and its symbol is 20px (Unicode ♍). Lying between Leo to the west and Libra to the east, it is the second-largest constellation in the sky (after Hydra) and the largest constellation in the zodiac. The ecliptic intersects the celestial equator within this constellation and Pisces.
The exact moment of a conjunction cannot be seen by every observer because the two planets are not in the sky for everybody. So the observer's location must be taken into account. So this third system takes in the closest point of an observer. This is usually very close to the calculated date and time in the ecliptic coordinate system.
Its orbit has an eccentricity of 0.43 and an inclination of 5° with respect to the ecliptic. It was first observed by the Near-Earth Asteroid Tracking on Palomar Observatory on 2 July 2002, or seven nights prior to its official discovery observation by LINEAR. This asteroid has an Earth minimum orbit intersection distance of , which corresponds to 2.7 lunar distances (LD).
Calandra is a non-family asteroid from the main belt's background population. It orbits the Sun in the outer main-belt at a distance of 2.7–3.4 AU once every 5 years and 4 months (1,952 days). Its orbit has an eccentricity of 0.12 and an inclination of 10° with respect to the ecliptic. No precoveries were taken prior to its discovery.
In between is the small faint emission nebula IC 444 around the 7th magnitude 12 Geminorum. η Geminorum is 0.9 degree south of the ecliptic, so it can be occulted by the Moon and, rarely, by planets. The last occultation by a planet took place on July 27, 1910, by Venus, and the next to last on July 11, 1837, by Mercury.
Epsilon Geminorum lies near the ecliptic, so it can be occulted by the Moon or a planet. Such an occultation took place on April 8, 1976 by Mars, which allowed the oblateness of the planet's outer atmosphere to be measured. Epsilon Geminorum was occulted by Mercury on June 10, 1940, and on September 3, 2015 it was occulted by the asteroid Iphigenia.
The Sun's gravitational attraction on the Moon pulls it toward the plane of the ecliptic, causing a slight wobble of about 9 arcmin within a 6-month period. In 2006, the effect of this was that, although the 18.6-year maximum occurred in June, the maximum declination of the Moon was not in June but in September, as shown in the third diagram.
Imaging Saturn (2016) is a multimedia installation that focuses on Saturn, its orbit, and the paths of the sun and surrounding stars. Incorporating aspects of participatory science and data visualization, the exhibit combines astronomy and astrophotography with mapping of Saturn's ecliptic, a mechanized orbiter (developed with Ray Peterson), kinetic sculptures, and video. It reflects an interest in Saturn going back to 2010.
The ecliptic and the meridian cut the sky into four quadrants. The axis of the earth wobbles around slowly moving the observer and changing the observation of the event. If the axis swings the observer closer to the event its observational year will be shortened. Likewise, the observational year can be lengthened when the axis swings away from the observer.
Eclipses occur when the three bodies form a nearly straight line. Because the plane of the lunar orbit is inclined to that of the Earth, this condition occurs only when a full or new Moon is near or in the ecliptic plane, that is when the Moon is at one of the two nodes (the ascending or descending node). The period of time for two successive lunar passes through the ecliptic plane (returning to the same node) is termed the draconic month, a 27.21222 day period. The three-dimensional geometry of an eclipse, when the new or full moon is near one of the nodes, occurs every five or six months when the Sun is in conjunction or opposition to the Moon and coincidentally also near a node of the Moon's orbit at that time, or twice per eclipse year.
This forms Michelson-like interferometers, each centred on one of the spacecraft, with the test masses defining the ends of the arms. The entire arrangement, which is ten times larger than the orbit of the Moon, will be placed in solar orbit at the same distance from the Sun as the Earth, but trailing the Earth by 20 degrees, and with the orbital planes of the three spacecraft inclined relative to the ecliptic by about 0.33 degree, which results in the plane of the triangular spacecraft formation being tilted 60 degrees from the plane of the ecliptic. The mean linear distance between the formation and the Earth will be 50 million kilometres. To eliminate non-gravitational forces such as light pressure and solar wind on the test masses, each spacecraft is constructed as a zero-drag satellite.
A special case of annual aberration is the nearly constant deflection of the Sun from its position in the Sun's rest frame by \kappa towards the west (as viewed from Earth), opposite to the apparent motion of the Sun along the ecliptic (which is from west to east, as seen from Earth). The deflection thus makes the Sun appear to be behind (or retarded) from its rest-frame position on the ecliptic by a position or angle \kappa. This deflection may equivalently be described as a light-time effect due to motion of the Earth during the 8.3 minutes that it takes light to travel from the Sun to Earth. The relation with κ is : [0.000099365 rad / 2 π rad] x [ 365.25 d x 24 h/d x 60 min/h] = 8.3 min = 8 min 19 s.
Pioneer H as it hangs in the National Air and Space Museum Pioneer H hangs in the Milestones of Flight Gallery at the National Air and Space Museum in Washington, D.C., serving as a stand-in for the Pioneer 10 probe. While described in official Smithsonian records as a "replica", the spacecraft was considered fully functional by Pioneer mission planners (though its RTGs were never installed). Mark Wolverton quotes James Van Allen in The Depths of Space: > We mounted an intensive campaign to launch the flight-worthy spare > spacecraft and its instrument complement on a low-cost, out-of-ecliptic > mission via a high-inclination flyby of Jupiter. However, our case fell on > deaf ears at NASA headquarters, and the spare spacecraft now hangs in the > main gallery of the National Air and Space Museum, at 1 AU and zero ecliptic > latitude.
The motion of the solar system, and the orientation of the plane of the ecliptic are aligned with features of the microwave sky, which on conventional thinking are caused by structure at the edge of the observable universe.CERN Courier "Does the motion of the solar system affect the microwave sky?" preprint Specifically, with respect to the ecliptic plane the "top half" of the CMB is slightly cooler than the "bottom half"; furthermore, the quadrupole and octupole axes are only a few degrees apart, and these axes are aligned with the top/bottom divide. Lawrence Krauss is quoted as follows in a 2006 Edge.org article: > But when you look at CMB map, you also see that the structure that is > observed, is in fact, in a weird way, correlated with the plane of the earth > around the sun.
Lindelöf orbits the Sun in the central main-belt at a distance of 2.0–3.5 AU once every 4 years and 7 months (1,680 days). Its orbit has an eccentricity of 0.28 and an inclination of 6° with respect to the ecliptic. In 1905, it was first identified as at Heidelberg Observatory, extending the body's observation arc by 31 years prior to its official discovery observation.
Explorer 47 continued the study begun by earlier IMP spacecraft of the interplanetary and magnetotail regions from a nearly circular orbit, near 37 earth radii. This 16 sided drum- shaped spacecraft was high and in diameter. It was designed to measure energetic particles, plasma and electric and magnetic fields. The spin axis was normal to the ecliptic plane, and the spin period was 1.3 s.
The supermoon of 14 November 2016 was away from the center of Earth. This occurrence happens yearly with the next one in 2020, the previous being in 2018. The full Moon of 22 October 2010, as seen through a Schmidt-Cassegrain telescope. This full Moon was near its northernmost ecliptic latitude (or northern lunistice), so the southern craters are especially prominent and cast shadows visible from Earth.
Explorer 41 was a spin-stabilized satellite placed into a high-inclination, highly elliptical orbit to measure energetic particles, magnetic fields, and plasma in cislunar space. The line of apsides and the satellite spin vector were within a few degrees of being parallel and normal, respectively, to the ecliptic plane. Initial local time of apogee was about 1,300 hours. Initial satellite spin rate was 27.5 rpm.
A modeled lightcurve gave a concurring sidereal period of 5.94819 hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys . The study also determined two spin axes of (183.0°, −50.0°) and (41.0°, −39.0°) in ecliptic coordinates (λ, β).
Philophrosyne is about 2 kilometres in diameter, and orbits Jupiter at an average distance of 22,721,000 km in 699.676 days, at an inclination of 142° to the ecliptic (142° to Jupiter's equator), in a retrograde direction and with an eccentricity of 0.0932. It belongs to the Pasiphae group, retrograde irregular moons that orbit Jupiter between 22.8 and 24.1 Gm, at inclinations of roughly 150-155°.
Its orbit has an eccentricity of 0.21 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins with the first recorded observation by the MPC at Vienna Observatory on 10 September 1885, or more than 9 years after its official discovery observation at Clinton. On 19 October 2005, it was observed occulting the prominent star Regulus from Vibo Valentia, Italy.
' is a minor planet and the first Neptune trojan discovered on 21 August 2001, by the Deep Ecliptic Survey at Cerro Tololo Observatory in Chile. It orbits ahead of Neptune at its Lagrangian point. Other Neptune trojans have been discovered since. A study by American astronomers Scott Sheppard and Chad Trujillo from the Carnegie Institution suggests that Neptune could possibly have twenty times more trojans than Jupiter.
Simulated view of Charon transiting Pluto on 25 February 1989. Transits occur when one of Pluto's moons passes between Pluto and the Sun. This occurs when one of the satellites' orbital nodes (the points where their orbits cross Pluto's ecliptic) lines up with Pluto and the Sun. This can only occur at two points in Pluto's orbit; coincidentally, these points are near Pluto's perihelion and aphelion.
These divisions were also used in scientific astronomy until the 19th century in some cases; see ecliptic coordinates. The concept of the zodiac originated in Babylonian astrology, and was later influenced by Hellenistic culture. According to astrology, celestial phenomena relate to human activity on the principle of "as above, so below", so that the signs are held to represent characteristic modes of expression.Mayo (1979), p. 35.
Bydžovský orbits the Sun in the outer main-belt at a distance of 2.7–3.3 AU once every 5 years and 3 months (1,923 days). Its orbit has an eccentricity of 0.09 and an inclination of 10° with respect to the ecliptic. It was first identified as at Heidelberg Observatory in 1950, extending the body's observation arc by 32 years prior to its discovery.
Animation of 1620 Geographos orbit 2010-2020 Geographos orbits the Sun at a distance of 0.8–1.7 AU once every 1 years and 5 months (508 days). Its orbit has an eccentricity of 0.34 and an inclination of 13° with respect to the ecliptic. Its orbit is well-determined for the next several hundred years. Due to its high eccentricity, Geographos is also a Mars-crosser asteroid.
Bobstephens orbits the Sun in the central main-belt at a distance of 2.0–3.2 AU once every 4 years and 2 months (1,523 days). Its orbit has an eccentricity of 0.22 and an inclination of 5° with respect to the ecliptic. It was first imaged at Steward Observatory in 1995. This precovery extends the body's observation arc by 3 years prior to its official discovery observation.
Bolyai orbits the Sun in the central main-belt at a distance of 2.0–3.3 AU once every 4 years and 3 months (1,559 days). Its orbit has an eccentricity of 0.24 and an inclination of 14° with respect to the ecliptic. Bolyais observation arc begins the night following its official discovery observation in 1937, as no precoveries were taken, and no prior identifications were made.
Bourgeois is a non-family asteroid from the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 1.8–3.5 AU once every 4 years and 3 months (1,561 days). Its orbit has an eccentricity of 0.32 and an inclination of 11° with respect to the ecliptic. The asteroid was first identified as at Johannesburg Observatory in June 1911.
The asteroid orbits the Sun at a distance of 0.8–1.7 AU once every 17 months (509 days). Its orbit has an eccentricity of 0.32 and an inclination of 15° with respect to the ecliptic. Its Earth minimum orbit intersection distance is . This makes the body a potentially hazardous asteroid, because its MOID is less than 0.05 AU and its diameter is greater than 150 meters.
Kagayayutaka is a non-family asteroid from the main belt's background population. It orbits the Sun in the outer main-belt at a distance of 2.5–3.6 AU once every 5 years and 5 months (1,984 days). Its orbit has an eccentricity of 0.18 and an inclination of 8° with respect to the ecliptic. The body's observation arc starts with its official discovery observation.
Jeffwynn is a stony asteroid that orbits the Sun at a distance of 1.6–3.1 AU once every 3 years and 7 months (1,307 days). Its orbit has an eccentricity of 0.32 and an inclination of 22° with respect to the ecliptic. The body's observation arc begins 36 years prior to its official discovery observation, with its precovery identification as at Palomar in July 1951.
Using observations of the comet over 102 days, Felix Körber was able to calculate only a parabolic orbit, inclined to the ecliptic by about 92°. The comet reached its perihelion of approximately 0.026 AU on January 14 and then on January 15 its closest approach to planet Earth of approximately 0.94 AU. On January 16 the comet passed by Venus at a distance of approximately 0.67 AU.
Inkeri is a non-family asteroid from the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.2–3.2 AU once every 4 years and 5 months (1,601 days). Its orbit has an eccentricity of 0.19 and an inclination of 7° with respect to the ecliptic. The asteroid was first identified as at Simeiz Observatory in January 1916.
It orbits the Sun in the central main- belt at a distance of 2.1–3.0 AU once every 4 years and 1 month (1,495 days). Its orbit has an eccentricity of 0.18 and an inclination of 9° with respect to the ecliptic. Innes was first identified as at Turku Observatory in 1940, extending the body's observation arc by 13 years prior to its official discovery observation.
Frisia is a Themistian asteroid that belongs to the Themis family (), a very large family of carbonaceous asteroids, named after 24 Themis. It orbits the Sun in the outer main-belt at a distance of 2.5–3.8 AU once every 5 years and 7 months (2,054 days). Its orbit has an eccentricity of 0.21 and an inclination of 1° with respect to the ecliptic.
Gawain orbits the Sun in the outer main-belt at a distance of 2.7–3.3 AU once every 5 years and 1 month (1,865 days). Its orbit has an eccentricity of 0.10 and an inclination of 4° with respect to the ecliptic. The asteroid's observation arc begins 6 years prior to its official discovery observation, with a precovery taken at the discovering Palomar Observatory in July 1954.
Haltia is a non-family asteroid of the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.1–3.0 AU once every 4 years and 1 month (1,481 days). Its orbit has an eccentricity of 0.19 and an inclination of 7° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Turku.
Golia orbits the Sun in the central main-belt at a distance of 2.3–2.9 AU once every 4 years and 2 months (1,516 days). Its orbit has an eccentricity of 0.11 and an inclination of 10° with respect to the ecliptic. The body's observation arc begins at Johannesburg one night after its official discovery observation, with no precoveries taken and no prior identifications made.
Gonnessia is not a member of any known asteroid family. It orbits the Sun in the outer main-belt at a distance of 3.2–3.5 AU once every 6 years and 2 months (2,238 days). Its orbit has an eccentricity of 0.03 and an inclination of 15° with respect to the ecliptic. The asteroid was first observed as at Simeiz Observatory in September 1923.
Gagarin orbits the Sun in the central main-belt at a distance of 2.3–2.8 AU once every 4.02 years (1,467 days). Its orbit has an eccentricity of 0.11 and an inclination of 6° with respect to the ecliptic. Gagarin first observation is a precovery that was taken at Turku Observatory in 1940, extending the body's observation arc by 28 years prior to its official discovery observation.
Holt orbits the Sun in the inner main-belt at a distance of 1.5–3.1 AU once every 3 years and 6 months (1,288 days). Its orbit has an eccentricity of 0.34 and an inclination of 22° with respect to the ecliptic. The first precovery was taken at Crimea-Nauchnij in 1978, extending the asteroid's observation arc by 5 years prior to its discovery.
ITA orbits the Sun in the outer main- belt at a distance of 2.7–3.5 AU once every 5 years and 7 months (2,030 days). Its orbit has an eccentricity of 0.13 and an inclination of 16° with respect to the ecliptic. It was first identified as at Heidelberg Observatory in 1907, extending the body's observation arc by 41 years prior to its official discovery observation.
3122 Florence is a stony trinary asteroid of the Amor group. It is classified as a near-Earth object and potentially hazardous asteroid. It measures approximately 5 kilometers in diameter. It orbits the Sun at a distance of 1.0–2.5 AU once every 2 years and 4 months (859 days); the orbit has an eccentricity of 0.42 and an inclination of 22° with respect to the ecliptic.
Deflotte is a non-family asteroid from the main belt's background population. It orbits the Sun in the outer main-belt at a distance of 3.0–3.8 AU once every 6 years and 3 months (2,281 days). Its orbit has an eccentricity of 0.12 and an inclination of 3° with respect to the ecliptic. The asteroid was first identified as at Heidelberg Observatory in September 1932.
Cassini is a non-family from the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 1.8–3.5 AU once every 4 years and 4 months (1,571 days). Its orbit has an eccentricity of 0.31 and an inclination of 15° with respect to the ecliptic. In December 1926, the asteroid was first identified as ' at Heidelberg Observatory in Germany.
Elatus orbits the Sun at a distance of 7.3–16.3 AU once every 40 years and 7 months (14,826 days). Its orbit has an eccentricity of 0.38 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins with a precovery taken by the Sloan Digital Sky Survey at Apache Point Observatory in September 1998, thirteen months prior to its official discovery observation.
Estonia is a non-family asteroid from the main belt's background population. It orbits the Sun in the central main belt at a distance of 2.6–3.0 AU once every 4 years and 7 months (1,683 days). Its orbit has an eccentricity of 0.07 and an inclination of 5° with respect to the ecliptic. The asteroid was first identified as at the Simeiz Observatory in April 1916.
Several rotational lightcurves of Antwerpia have been obtained from photometric observations since 2005. Lightcurve analysis gave a rotation period of 6.63 hours with a brightness variation of 0.42 magnitude (). A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database (LPD), gave a concurring period of 6.62521 hours (), as well as two spin axis of (128.0°, −66.0°) and (246.0°, −76.0°) in ecliptic coordinates (λ, β).
Ambartsumian orbits the Sun in the inner main-belt at a distance of 1.9–2.6 AU once every 3 years and 4 months (1,211 days). Its orbit has an eccentricity of 0.16 and an inclination of 3° with respect to the ecliptic. It was first identified as at Simeiz Observatory in 1932, extending the body's observation arc by 40 years prior to its official discovery observation.
Angola orbits the Sun in the outer main-belt at a distance of 2.7–3.6 AU once every 5 years and 8 months (2,058 days). Its orbit has an eccentricity of 0.15 and an inclination of 19° with respect to the ecliptic. Angola was first identified as at Johannesburg in 1929, extending the body's observation arc by 6 years prior to its official discovery observation.
Alexisrodrz orbits the Sun in the central main-belt at a distance of 2.5–2.8 AU once every 4 years and 3 months (1,565 days). Its orbit has an eccentricity of 0.06 and an inclination of 6° with respect to the ecliptic. The asteroid's observation arc begins 7 years prior to its official discovery observation, with a precovery taken at Steward Observatory (Kitt Peak) in November 1992.
This asteroid orbits the Sun in the outer main-belt at a distance of 2.9–3.5 AU once every 5 years and 9 months (2,101 days). Its orbit has an eccentricity of 0.08 and an inclination of 17° with respect to the ecliptic. Alikoskis observation arc begins with a precovery taken at Turku in 1938, extending it by 3 years prior to the asteroid's official discovery observation.
Alpaidze is a non-family asteroid from the main belt's background population. It orbits the Sun in the central main-belt at a distance of 1.8–3.4 AU once every 4 years and 3 months (1,563 days). Its orbit has an eccentricity of 0.31 and an inclination of 2° with respect to the ecliptic. It was first identified as ' at Palomar Observatory in November 1978.
This asteroid orbits the Sun in the outer main-belt at a distance of 2.8–3.6 AU once every 5 years and 9 months (2,091 days). Its orbit has an eccentricity of 0.13 and an inclination of 13° with respect to the ecliptic. Alschmitt was first identified as at Heidelberg in 1906, extending the body's observation arc by 46 years prior to its official discovery observation.
The S-type asteroid is a member of the Flora family, one of the largest groups of stony asteroids in the main- belt. It orbits the Sun in the inner main-belt at a distance of 1.9–2.6 AU once every 3 years and 5 months (1,238 days). Its orbit has an eccentricity of 0.15 and an inclination of 8° with respect to the ecliptic.
The C-type asteroid orbits the Sun in the inner main-belt at a distance of 2.0–2.8 AU once every 3 years and 8 months (1,339 days). Its orbit has an eccentricity of 0.17 and an inclination of 3° with respect to the ecliptic. The first precovery was obtained at El Leoncito in 1975, extending the asteroid's observation arc by 7 years prior to its discovery.
Brahms orbits the Sun in the inner main-belt at a distance of 1.8–2.6 AU once every 3 years and 2 months (1,163 days). Its orbit has an eccentricity of 0.18 and an inclination of 3° with respect to the ecliptic. Brahms was first identified as at the discovering observatory in 1904, extending the body's observation arc by 35 years prior to its official discovery observation.
Brucemurray orbits the Sun at a distance of 1.2–1.9 AU once every 1 years and 12 months (715 days). Its orbit has an eccentricity of 0.22 and an inclination of 35° with respect to the ecliptic. The body's observation arc begins with a precovery taken at the Australian Siding Spring Observatory in March 1976, or more than 14 years prior to its official discovery observation.
The S-type asteroid is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbit has an eccentricity of 0.13 and an inclination of 2° with respect to the ecliptic. As no precovery were taken, and no prior identifications were made, the body's observation arc begins with its official discovery observation at Palomar in 1960.
Pemba is a non-family asteroid from the main belt's background population. It orbits the Sun in the central main-belt at a distance of 1.7–3.4 AU once every 4 years and 1 month (1,492 days). Its orbit has an eccentricity of 0.33 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Johannesburg.
Photometric observations of Prisma gave a well defined rotational lightcurve with a period between 6.546 and 6.558 hours and a high brightness variation of 0.85–1.16 magnitude, which strongly indicates that the body has an elongated, non-spheroidal shape (). A modeled lightcurve based on optical data from a large collaboration network also found a spin axis of (133.0°, −78.0°) in ecliptic coordinates (λ, β) ().
Pskov orbits the Sun in the central main-belt at a distance of 2.1–3.3 AU once every 4 years and 6 months (1,657 days). Its orbit has an eccentricity of 0.22 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins 27 years prior to its official discovery observation, with a precovery taken at Palomar Observatory in November 1955.
Rafita asteroid orbits the Sun in the central main-belt at a distance of 2.2–2.9 AU once every 4 years and 1 month (1,486 days). Its orbit has an eccentricity of 0.15 and an inclination of 7° with respect to the ecliptic. Rafita was first observed as at Heidelberg Observatory in 1906, extending the body's observation arc by 29 years prior to its official discovery observation.
Kugultinov is a carbonaceous C-type asteroid and member of the Themis family, a dynamical family of outer-belt asteroids with nearly coplanar ecliptical orbits. It orbits the Sun in the outer main-belt at a distance of 2.7–3.7 AU once every 5 years and 8 months (2,073 days). Its orbit has an eccentricity of 0.17 and an inclination of 1° with respect to the ecliptic.
Karge orbits the Sun in the inner main-belt at a distance of 1.8–2.7 AU once every 3 years and 5 months (1,235 days). Its orbit has an eccentricity of 0.19 and an inclination of 4° with respect to the ecliptic. first precovery was taken at the Palomar Observatory in 1971, extending the body's observation arc by 15 years prior to its official discovery observation.
Kate orbits the Sun in the inner main-belt at a distance of 1.8–2.7 AU once every 3 years and 4 months (1,226 days). Its orbit has an eccentricity of 0.20 and an inclination of 5° with respect to the ecliptic. As no precoveries were taken, and no prior identifications were made, the asteroid's observation arc begins with its official discovery observation at Simeiz in 1917.
Tesla orbits the Sun in the central main-belt at a distance of 2.3–3.3 AU once every 4 years and 9 months (1,721 days). Its orbit has an eccentricity of 0.18 and an inclination of 8° with respect to the ecliptic. It was first identified as at Turku Observatory in 1938, extending the body's observation arc by 14 years prior to its official discovery at Belgrade.
The presumably stony asteroid orbits the Sun in the central main-belt at a distance of 2.4–3.0 AU once every 4 years and 5 months (1,600 days). Its orbit has an eccentricity of 0.11 and an inclination of 4° with respect to the ecliptic. First identified as at Uccle Observatory in 1934, Klares observation arc begins 20 years prior to its official discovery observation.
Lugano is a member of the Adeona family (), a large family of carbonaceous asteroids. It orbits the Sun in the central main-belt at a distance of 2.3–3.0 AU once every 4 years and 5 months (1,599 days). Its orbit has an eccentricity of 0.14 and an inclination of 10° with respect to the ecliptic. It was first identified as at Johannesburg Observatory in 1936.
Lomonosowa is a non-family asteroid of the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.3–2.8 AU once every 4.01 years (1,464 days). Its orbit has an eccentricity of 0.09 and an inclination of 16° with respect to the ecliptic. The body's observation arc begins with its first precovery at Lowell Observatory in October 1905.
Limpopo orbits the Sun in the inner main-belt at a distance of 2.0–2.7 AU once every 3 years and 7 months (1,318 days). Its orbit has an eccentricity of 0.16 and an inclination of 10° with respect to the ecliptic. The body's observation arc begins 2 weeks prior to its official discovery observation. Its first identification as at Lowell Observatory in 1931 remains unused.
Modelling gave a concurring (sidereal) period of 4.679100, 4.679102 and 4.67911 hours. The studies determined two spin axis in ecliptic coordinates (λ, β): (73.0°, −54.0°) and (198.0°, −55.0°), as well as (72.0°, −59.0°) and (207.0°, −51.0°). Modeling also confirmed that the body is a slightly elongated ellipsoid, and revealed that it is rotating along the smallest axis and that it has an almost homogeneous surface.
Marilyn is a non-family asteroid from the main belt's background population. It orbits the Sun in the inner asteroid belt at a distance of 1.9–2.5 AU once every 3 years and 3 months (1,191 days). Its orbit has an eccentricity of 0.12 and an inclination of 0° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Uccle.
Leuschneria is a carbonaceous C-type asteroid that orbits the Sun at a distance of 2.7–3.5 AU once every 5 years and 5 months (1,976 days). Its orbit has an eccentricity of 0.13 and an inclination of 22° with respect to the ecliptic. It was first observed at Johannesburg Observatory, extending the body's observation arc by 3 days prior to its official discovery observation at Uccle.
This asteroid orbits the Sun in the outer main-belt at a distance of 2.6–3.1 AU once every 4 years and 10 months (1,752 days). Its orbit has an eccentricity of 0.09 and an inclination of 12° with respect to the ecliptic. As no precoveries were taken and no prior identifications were made, Laugiers observation arc begins with its official discovery observation in 1949.
Lacroute orbits the Sun in the outer main-belt at a distance of 2.5–3.7 AU once every 5 years and 6 months (1,996 days). Its orbit has an eccentricity of 0.19 and an inclination of 2° with respect to the ecliptic. As no precoveries were taken, and no prior identifications were made, the body's observation arc begins with its official discovery observation in 1950.
Massachusetts is a non-family asteroid of the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.4–2.8 AU once every 4 years and 3 months (1,543 days). Its orbit has an eccentricity of 0.07 and an inclination of 18° with respect to the ecliptic. The asteroid was first observed as at Crimea-Nauchnij in October 1969.
Massevitch orbits the Sun in the central main-belt at a distance of 2.5–2.9 AU once every 4 years and 7 months (1,662 days). Its orbit has an eccentricity of 0.07 and an inclination of 13° with respect to the ecliptic. It was first identified as at Goethe Link Observatory in 1949, extending the body's observation arc by 23 years prior to its discovery observation.
Nocturna is a non-family asteroid of the main belt's background population. It orbits the Sun in the outer asteroid belt at a distance of 2.7–3.6 AU once every 5 years and 6 months (2,018 days). Its orbit has an eccentricity of 0.15 and an inclination of 5° with respect to the ecliptic. The asteroid was first identified as at Heidelberg in September 1904.
Ruppina asteroid orbits the Sun in the outer main-belt at a distance of 2.7–3.1 AU once every 5.04 years (1,840 days). Its orbit has an eccentricity of 0.06 and an inclination of 2° with respect to the ecliptic. In 1931, Ruppina was first identified as at Lowell Observatory, extending the body's observation arc by 6 years prior to its official discovery at Heidelberg.
Several rotational lightcurve of Rosselia have been obtained from photometric observations since 1975. Consolidated lightcurve-analysis gave a well-defined rotation period of 8.140 hours with a brightness amplitude between 0.3 and 0.54 magnitude (). Modeling of the asteroid's lightcurve gave two concurring periods of 8.14008 and 8.14011 hours, with two determined spin axis of (67.0°, −64.0°) and (246.0°, −58.0°) in ecliptic coordinates (λ, β).
Rovaniemi is a member of the Flora family (), a giant asteroid family and the largest family of stony asteroids in the main-belt. It orbits the Sun in the inner main-belt at a distance of 1.9–2.5 AU once every 3 years and 4 months (1,212 days). Its orbit has an eccentricity of 0.14 and an inclination of 7° with respect to the ecliptic.
His Quadripartitum was the first text on spherical trigonometry to be published in Western Europe. The rectangulus was a form of skeleton torquetum. This was a series of nested angular scales, so that measurements in azimuth and elevation could be made directly in polar coordinates, relative to the ecliptic. Conversion from these coordinates though was difficult, involving what was the leading mathematics of the day.
Animated orbit of Hygiea relative to the orbits of the terrestrial planets and Jupiter. Orbiting at an average of 3.14 AU from the Sun, Hygiea is the most distant of the "big four" asteroids. It lies closer to the ecliptic as well, with an orbital inclination of 4°. Its orbit is less circular than those of Ceres or Vesta, with an eccentricity of around 0.12.
Also with the introduction of the International Celestial Reference Frame, all objects near and far are put fundamentally in relationship to a large frame based on very distant fixed radio sources, and the choice of the origin is arbitrary and defined for the convenience of the problem at hand. There are no significant problems in astronomy where the ecliptic and the equinox need to be defined.
Amaryllis is a non-family asteroid from the main belt's background population. It orbits the Sun in the outer asteroid belt at a distance of 3.1–3.3 AU once every 5 years and 8 months (2,076 days). Its orbit has an eccentricity of 0.04 and an inclination of 7° with respect to the ecliptic. The asteroid was first identified as at Taunton Observatory () in April 1908.
Beljawskya is a member of the Themis family, a dynamical family of outer-belt asteroids with nearly coplanar ecliptical orbits. It orbits the Sun at a distance of 2.6–3.7 AU once every 5 years and 7 months (2,042 days). Its orbit has an eccentricity of 0.18 and an inclination of 1° with respect to the ecliptic. It was first identified as at Winchester Observatory () in 1912.
Božněmcová orbits the Sun in the central main-belt at a distance of 1.8–3.3 AU once every 4.04 years (1,477 days). Its orbit has an eccentricity of 0.30 and an inclination of 7° with respect to the ecliptic. It was first identified as at Lowell Observatory in 1930, extending the body's observation arc by 49 years prior to its official discovery observation at Klet.
Enya is a non-family asteroid from the main belt's background population. It orbits the Sun in the inner asteroid belt at a distance of 1.9–2.9 AU once every 3 years and 8 months (1,348 days). Its orbit has an eccentricity of 0.22 and an inclination of 9° with respect to the ecliptic. Enya was first identified as at Goethe Link Observatory in 1952.
The orbit of along with other Haumea family objects orbits the Sun at a distance of 38.3–49.8 AU once every 292 years and 5 months (semi-major axis of 44.05 AU). Its orbit has an eccentricity of 0.13 and an inclination of 27° with respect to the ecliptic. Precovery images have been identified back to 2002. Estimates for its diameter range between 138 and 423 kilometers.
Rupertwildt orbits the Sun in the outer main-belt at a distance of 2.5–3.7 AU once every 5 years and 6 months (2,003 days). Its orbit has an eccentricity of 0.18 and an inclination of 2° with respect to the ecliptic. Due to a precovery taken at Lowell Observatory in 1929, the asteroid's observation arc begins 22 years before its official discovery observation at Goethe Link.
Hesburgh orbits the Sun in the outer main-belt at a distance of 2.7–3.6 AU once every 5 years and 6 months (2,005 days). Its orbit has an eccentricity of 0.14 and an inclination of 14° with respect to the ecliptic. It was first identified as at Johannesburg Observatory in 1936. The body's observation arc begins at Goethe, five days after its official discovery observation.
Alisondoane is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner main-belt at a distance of 1.8–3.1 AU once every 3 years and 10 months (1,397 days). Its orbit has an eccentricity of 0.26 and an inclination of 6° with respect to the ecliptic.
Bancilhon orbits the Sun in the inner main-belt at a distance of 1.8–2.6 AU once every 3 years and 4 months (1,215 days). Its orbit has an eccentricity of 0.18 and an inclination of 4° with respect to the ecliptic. It was first identified as at Lowell Observatory in 1931, extending the body's observation arc by 20 years prior to its official discovery observation.
Barney is a core member of the Maria family (), a large intermediate belt family of stony asteroids. It orbits the Sun in the central main-belt at a distance of 2.5–2.7 AU once every 4 years and 2 months (1,512 days; semi-major axis of 2.58 AU). Its orbit has an eccentricity of 0.04 and an inclination of 14° with respect to the ecliptic.
It orbits the Sun in the middle main-belt at a distance of 2.1–3.4 AU once every 4 years and 8 months (1,695 days). Its orbit has an eccentricity of 0.24 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Palomar, as no precoveries were taken, and no prior identifications were made.
The S-type asteroid orbits the Sun at a distance of 1.9–2.9 AU once every 3 years and 7 months (1,322 days). Its orbit has an eccentricity of 0.21 and an inclination of 1° with respect to the ecliptic. The first observation was made at the U.S. Yerkes Observatory in 1931, extending the asteroid's observation arc by 55 years prior to its official discovery.
Pólit orbits the Sun in the outer main-belt at a distance of 2.0–3.8 AU once every 4 years and 12 months (1,814 days). Its orbit has an eccentricity of 0.31 and an inclination of 6° with respect to the ecliptic. A first precovery was taken at Lowell Observatory in Flagstaff, extending the body's observation arc by 3 days prior to its official discovery observation.
In October 2010, a rotational lightcurve of Seinäjoki was obtained by Russell Durkee at the U.S. Shed of Science Observatory () in Minneapolis. It gave it a well- defined rotation period of 4.32 hours with a brightness variation of 0.15 magnitude (). A modeled lightcurve form Lowell photometric database gave a concurring period of 4.328 hours and a spin axis of (-18.0°, 230.0°) in ecliptic coordinates.
The dark C-type asteroid is a member of the Themis family, a dynamical family of outer-belt asteroids with nearly coplanar ecliptical orbits. It orbits the Sun in the outer main-belt at a distance of 2.6–3.7 AU once every 5 years and 7 months (2,029 days). Its orbit has an eccentricity of 0.18 and an inclination of 2° with respect to the ecliptic.
Strömgrenia is a member of the Flora family, a large group of stony asteroids in the inner main-belt. It orbits the Sun at a distance of 1.9–2.6 AU once every 3 years and 4 months (1,230 days). Its orbit has an eccentricity of 0.17 and an inclination of 3° with respect to the ecliptic. It was first identified as at Uccle Observatory in 1933.
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It lies near the ecliptic and thus is subject to occultation by the Moon. One such event was observed September 3, 1991. This system forms a wide double star with an angular separation of along a position angle of 230°, as of 1991. The brighter star, component A, has an apparent magnitude of 4.99 while the fainter secondary, component B, is of magnitude 9.09.
75 Tauri is a single, orange-hued star in the zodiac of constellation Taurus. It is a dim star but visible to the naked eye with an apparent visual magnitude of 4.96. Based upon an annual parallax shift of 17.47 mas as seen from Earth's orbit, it is located around 187 light years away. Due to its position near the ecliptic, it is subject to lunar occultations.
Tiziano orbits the Sun in the inner main-belt at a distance of 2.1–2.7 AU once every 3 years and 9 months (1,361 days). Its orbit has an eccentricity of 0.13 and an inclination of 13° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Palomar, as no precoveries were taken, and no prior identifications were made.
Raïssa is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 2.2–2.7 AU once every 3 years and 9 months (1,378 days). Its orbit has an eccentricity of 0.10 and an inclination of 4° with respect to the ecliptic.
Attica orbits the Sun in the outer main-belt at a distance of 2.9–3.4 AU once every 5 years and 7 months (2,037 days). Its orbit has an eccentricity of 0.07 and an inclination of 14° with respect to the ecliptic. The body's observation arc begins at Heidelberg with its official discovery observation. No precoveries were taken, and no prior identifications were made.
Hollandia is an assumed stony S-type asteroid. It orbits the Sun at a distance of 1.9–3.4 AU once every 4 years and 5 months (1,609 days). Its orbit has an eccentricity of 0.278 and an inclination of 7° with respect to the ecliptic. The body's observation arc begins with its official discovery observation as no precoveries were taken and no prior identifications were made.
Biarmia is not a member of any known asteroid family. It orbits the Sun in the outer main-belt at a distance of 2.3–3.8 AU once every 5 years and 4 months (1,940 days). Its orbit has an eccentricity of 0.26 and an inclination of 17° with respect to the ecliptic. The asteroid was first identified as at Winchester Observatory () in June 1913.
Pawona is a supposed member of the stony Vesta family (), named after 4 Vesta and the main belt's second-largest asteroid family by number. It orbits the Sun in the inner main-belt at a distance of 2.3–2.5 AU once every 3 years and 9 months (1,381 days). Its orbit has an eccentricity of 0.04 and an inclination of 5° with respect to the ecliptic.
Luda orbits the Sun at a distance of 2.3–2.9 AU once every 4 years and 1 month (1,499 days). Its orbit has an eccentricity of 0.11 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins with its first used observation at Johannesburg Observatory, one month after its official discovery observation at Simeiz. Luda is a stony S-type asteroid.
The dark C-type asteroid is not a member of any known asteroid family. It orbits the Sun in the outer main-belt at a distance of 3.1–3.3 AU once every 5 years and 9 months (2,113 days). Its orbit has an eccentricity of 0.03 and an inclination of 10° with respect to the ecliptic. Järnefelt was first identified as at Heidelberg in 1913.
Kubáček orbits the Sun in the central main-belt at a distance of 2.3–2.8 AU once every 4 years and 1 month (1,501 days). Its orbit has an eccentricity of 0.10 and an inclination of 5° with respect to the ecliptic. Its observation arc begins 10 years prior to its official discovery observation, with its identification as at the French Caussols Observatory in February 1987.
Titius orbits the Sun in the inner main-belt at a distance of 2.3–2.6 AU once every 3 years and 9 months (1,375 days). Its orbit has an eccentricity of 0.06 and an inclination of 8° with respect to the ecliptic. It stays in a 2:1 orbital resonance with the planet Mars. Titius observation arc starts on the night following its official discovery observation.
From initial observations of the spectrum, it was estimated that both components were giants and that the secondary was itself double. Radial velocity variations had been found in 1906, but only one set of absorption lines could be detected in the spectrum and it was not possible to calculate a reliable orbit until 1976. 1 Geminorum is a triple star system 0.17 degree south of the ecliptic.
Since 2004, several rotational lightcurves of Lilofee were obtained from photometric observations by astronomers René Roy, Enric Forné and Robert Stephens. Lightcurve analysis gave a rotation period of 8.255 hours with a brightness variation of 0.57 magnitude (). In 2013, an international study modeled a lightcurve with a concurring period of 8.24991 hours and found a spin axis of (n.a., −99.0°) in ecliptic coordinates (λ, β).
The combination of this fine asteroid dust, as well as ejected cometary material, produces the zodiacal light. This faint auroral glow can be viewed at night extending from the direction of the Sun along the plane of the ecliptic. Asteroid particles that produce the visible zodiacal light average about 40 μm in radius. The typical lifetimes of main-belt zodiacal cloud particles are about 700,000 years.
But still, Makemake's orbit is slightly farther from the Sun in terms of both the semi-major axis and perihelion. Its orbital period is 306 years, more than Pluto's 248 years and Haumea's 285 years. Both Makemake and Haumea are currently far from the ecliptic (at an angular distance of almost 29°). Makemake is approaching its 2033 aphelion, whereas Haumea passed its aphelion in early 1992.
The C-type asteroid orbits the Sun at a distance of 2.6–3.8 AU once every 5 years and 7 months (2,049 days). Its orbit has an eccentricity of 0.19 and an inclination of 18° with respect to the ecliptic. The first used observation was taken at the discovering observatory in 1913, extending the body's observation arc by 11 years prior to its discovery.
Semphyra has not been associated with any known asteroid family. It orbits the Sun in the central main belt at a distance of 2.2–3.4 AU once every 4 years and 8 months (1,714 days). Its orbit has an eccentricity of 0.20 and an inclination of 2° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Heidelberg.
O'Rourke orbits the Sun in the inner main-belt at a distance of 1.7–2.7 AU once every 3 years and 3 months (1,190 days). Its orbit has an eccentricity of 0.23 and an inclination of 5° with respect to the ecliptic. It was first observed as at Crimea–Nauchnij in 1975, extending the asteroid's observation arc by 6 years prior to its official discovery observation.
Many astronomical clocks use an astrolabe-style display, such as the famous clock at Prague, adopting a stereographic projection (see below) of the ecliptic plane. In recent times, astrolabe watches have become popular. For example, Swiss watchmaker Dr. Ludwig Oechslin designed and built an astrolabe wristwatch in conjunction with Ulysse Nardin in 1985. Dutch watchmaker Christaan van der Klauuw also manufactures astrolabe watches today.
Teutonia orbits the Sun in the central main-belt at a distance of 2.2–2.9 AU once every 4 years and 2 months (1,510 days). Its orbit has an eccentricity of 0.14 and an inclination of 4° with respect to the ecliptic. The asteroid's observation arc begin 17 years prior to its official discovery observation, with its first identification as at Taunton Observatory ( in March 1907.
Závist orbits the Sun in the central main-belt at a distance of 2.2–3.0 AU once every 4 years and 2 months (1,520 days). Its orbit has an eccentricity of 0.17 and an inclination of 11° with respect to the ecliptic. The first precovery was taken at Palomar Observatory in 1980, extending the asteroid's observation arc by 15 years prior to its discovery.
Nanna is a dark C-type asteroid. It orbits the Sun at a distance of 2.2–3.6 AU once every 4 years and 11 months (1,797 days). Its orbit has an eccentricity of 0.25 and an inclination of 6° with respect to the ecliptic. In 1926, it was first identified as , extending the body's observation arc by 5 years prior to its official discovery observation.
It orbits the Sun in the central main-belt at a distance of 2.2–2.9 AU once every 4 years and 1 month (1,499 days). Its orbit has an eccentricity of 0.15 and an inclination of 7° with respect to the ecliptic. The body's observation arc begins at the discovering Palomar Observatory on 7 October 1977, just 9 days prior to its official discovery observation.
Belgica is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbits the Sun at a distance of 1.9–2.6 AU once every 3 years and 4 months (1,222 days). Its orbit has an eccentricity of 0.14 and an inclination of 5° with respect to the ecliptic. Belgica was first identified as at Heidelberg in 1908.
Vogelweide is a stony asteroid and member of the Koronis family, a group consisting of few hundred known bodies with nearly ecliptical orbits. It orbits the Sun in the outer main-belt at a distance of 2.8–3.0 AU once every 4 years and 10 months (1,778 days). Its orbit has an eccentricity of 0.03 and an inclination of 3° with respect to the ecliptic.
Carestia orbits the Sun in the outer main-belt at a distance of 2.5–3.9 AU once every 5 years and 9 months (2,104 days). Its orbit has an eccentricity of 0.21 and an inclination of 21° with respect to the ecliptic. The first precovery was taken at Crimea-Simeis in 1939, extending the asteroid's observation arc by 38 years prior to its discovery.
' is a member of the Apollo asteroids, which cross the orbit of Earth. Apollo's are the largest group of near-Earth objects with nearly 10 thousand known objects. The object orbits the Sun at a distance of 0.87–1.17 AU once every 374 days (semi-major axis of 1.02 AU). Its orbit has an eccentricity of 0.15 and an inclination of 13° with respect to the ecliptic.
Cevasco orbits the Sun in the inner main-belt at a distance of 2.1–2.8 AU once every 3 years and 10 months (1,390 days). Its orbit has an eccentricity of 0.13 and an inclination of 1° with respect to the ecliptic. The asteroid's observation arc begins 6 years prior to its official discovery observation, with its first identification as at ESO's La Silla Observatory in 1993.
Pink Floyd is a non-family asteroid from the background population. It orbits the Sun in the inner main-belt at a distance of 2.0–2.8 AU once every 3 years and 10 months (1,397 days). Its orbit has an eccentricity of 0.16 and an inclination of 4° with respect to the ecliptic. The asteroid was first identified as at the discovering Caussols Observatory in October 1985.
Leleākūhonua orbits the Sun at a distance of once roughly every 32,000 years (semi-major axis of ~1080 AU). Its orbit has a very high eccentricity of 0.94 and an inclination of with respect to the ecliptic. It belongs to the extreme trans-Neptunian objects defined by their large semi-major axis and is the third sednoid ever to be discovered, after and ("Biden").
Acapulco is a member of the Adeona family (), a large family of carbonaceous asteroids. It orbits the Sun in the central main-belt at a distance of 2.3–3.0 AU once every 4 years and 4 months (1,590 days). Its orbit has an eccentricity of 0.14 and an inclination of 11° with respect to the ecliptic. In March 1947, it was first identified as at Yerkes Observatory.
Schumann orbits the Sun in the outer main-belt at a distance of 3.1–3.7 AU once every 6 years and 4 months (2,316 days). Its orbit has an eccentricity of 0.09 and an inclination of 5° with respect to the ecliptic. The first precovery was obtained at Heidelberg Observatory in 1933, extending the asteroid's observation arc by 31 years prior to its discovery.
Savonlinna orbits the Sun in the central main-belt at a distance of 2.0–3.4 AU once every 4 years and 5 months (1,620 days). Its orbit has an eccentricity of 0.26 and an inclination of 6° with respect to the ecliptic. It was first identified as at Simeiz Observatory, extending the body's arc length by 9 years prior to its official discovery observation at Turku.
Zephyr orbits the Sun at a distance of 1.0–2.9 AU once every 2 years and 9 months (1,003 days). Its orbit has an eccentricity of 0.49 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar Observatory in April 1955, almost 44 years prior to its official discovery observation at Anderson Mesa.
Zichichi is a S-type asteroid and member of the Flora family, one of the largest collisional populations of stony asteroids in the main-belt. It orbits the Sun in the inner main-belt at a distance of 1.9–2.7 AU once every 3 years and 7 months (1,307 days). Its orbit has an eccentricity of 0.17 and an inclination of 5° with respect to the ecliptic.
Yeomans is a non-family asteroid from the asteroid belt's background population. It orbits the Sun in the central main-belt at a distance of 2.5–3.0 AU once every 4 years and 7 months (1,679 days). Its orbit has an eccentricity of 0.09 and an inclination of 3° with respect to the ecliptic. The asteroid was first identified as at the Johannesburg Observatory in May 1950.
Whipple orbits the Sun in the outer main-belt at a distance of 2.9–3.3 AU once every 5 years and 4 months (1,956 days). Its orbit has an eccentricity of 0.06 and an inclination of 7° with respect to the ecliptic. The first used observation was made at Goethe Link Observatory in 1962, extending the asteroid's observation arc by 13 years prior to its discovery observation.
Stobbe orbits the Sun in the central main-belt at a distance of 2.6–2.7 AU once every 4 years and 3 months (1,540 days). Its orbit has an eccentricity of 0.02 and an inclination of 11° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Bergedorf. Its first (unused) identification as was made at Heidelberg Observatory in 1902.
The C-type asteroid is a non-family asteroid that belongs to the background population of the main belt. It orbits the Sun in the outer asteroid belt at a distance of 2.9–3.2 AU once every 5 years and 4 months (1,939 days; semi-major axis of 3.04 AU). Its orbit has an eccentricity of 0.05 and an inclination of 10° with respect to the ecliptic.
Mercury and Venus appears above the Moon, as viewed from the Paranal Observatory in northern Chile. In astronomy, a conjunction occurs when two astronomical objects or spacecraft have either the same right ascension or the same ecliptic longitude, usually as observed from Earth. The astronomical symbol for conjunction is ☌ (in Unicode U+260C) and handwritten 20px. The conjunction symbol is not used in modern astronomy.
Umtata is a non-family asteroid of the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.0–3.4 AU once every 4 years and 5 months (1,603 days). Its orbit has an eccentricity of 0.26 and an inclination of 4° with respect to the ecliptic. The asteroid was first identified as at the Lowell Observatory in April 1931.
Utopia is a non-family asteroid from the main belt's background population. It orbits the Sun in the outer asteroid belt at a distance of 2.7–3.5 AU once every 5 years and 6 months (2,010 days). Its orbit has an eccentricity of 0.12 and an inclination of 18° with respect to the ecliptic. The asteroid was first identified as at Simeiz Observatory in February 1930.
Soma is a member of the Flora family, a large family of stony asteroids. It orbits the Sun in the inner main-belt at a distance of 1.9–2.6 AU once every 3 years and 4 months (1,219 days). Its orbit has an eccentricity of 0.17 and an inclination of 6° with respect to the ecliptic. It was first identified as at Goethe Link Observatory in 1955.
Sootiyo orbits the Sun in the central main-belt at a distance of 2.0–3.2 AU once every 4 years and 3 months (1,537 days). Its orbit has an eccentricity of 0.22 and an inclination of 10° with respect to the ecliptic. The first used precovery was taken at Palomar Observatory in 1953, extending the asteroid's observation arc by 28 years prior to its discovery observation.
Varsavia orbits the Sun in the central main-belt at a distance of 2.2–3.2 AU once every 4 years and 4 months (1,589 days). Its orbit has an eccentricity of 0.19 and an inclination of 29° with respect to the ecliptic. As no precoveries were taken, and no prior identifications were made, the body's observation arc begins with its official discovery observation at Uccle in 1933.
Adamovich is a S-type asteroid a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbits the Sun in the inner main-belt at a distance of 1.8–2.6 AU once every 3 years and 3 months (1,175 days). Its orbit has an eccentricity of 0.20 and an inclination of 4° with respect to the ecliptic.
Arnolda is not a member of any known asteroid family. It orbits the Sun in the central main belt at a distance of 1.9–3.2 AU once every 4 years and 1 month (1,480 days). Its orbit has an eccentricity of 0.25 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins nine days prior to its official discovery observation at Heidelberg.
Due to this, as much as one quarter of the Trojans cannot intersect with the Hildas, and at all times many Trojans are located outside Jupiter's orbit. Therefore, the regions of intersection are limited. This is illustrated by the adjacent figure that shows the Hildas (black) and the Trojans (gray) along the ecliptic plane. One can see the spherical form of the Trojan swarms.
Justinehénin orbits the Sun in the outer main-belt at a distance of 2.8–3.6 AU once every 5 years and 9 months (2,091 days). Its orbit has an eccentricity of 0.12 and an inclination of 2° with respect to the ecliptic. The first identification was made at Crimea–Nauchnij in 1973, extending the asteroid's observation arc by 31 years prior to its discovery.
In 850, al-Farghani wrote Kitab fi Jawani ("A compendium of the science of stars"). The book primarily gave a summary of Ptolemic cosmography. However, it also corrected Ptolemy's Almagest based on findings of earlier Iranian astronomers. Al- Farghani gave revised values for the obliquity of the ecliptic, the precessional movement of the apogees of the sun and the moon, and the circumference of the earth.
It also possessed internal sensors enabling it to detect heat. In its second form, the android Taurus had enhanced strength and was immune to energy blasts. The Ecliptic version of Taurus had superhuman strength and carried the Zodiac teleportation device. Thanos' Taurus wears a special suit given to him by Thanos which enables him to possess super-strength and transform into a minotaur-like form.
In 850, al- Farghani wrote Kitab fi Jawami (meaning "A compendium of the science of stars"). The book primarily gave a summary of Ptolemic cosmography. However, it also corrected Ptolemy based on findings of earlier Arab astronomers. Al- Farghani gave revised values for the obliquity of the ecliptic, the precessional movement of the apogees of the Sun and the Moon, and the circumference of the Earth.
The object is located in the "gap", a poorly understood region. orbits the Sun at a distance of 50.8–74.8 AU once every 497 years and 10 months (181,824 days; semi-major axis of 62.81 AU). Its orbit has an eccentricity of 0.19 and an inclination of 35° with respect to the ecliptic. The object belongs to the same group as ("Buffy"), , and (also see diagram).
The object is located in the "gap", a poorly understood region. orbits the Sun at a distance of 51.7–100.6 AU once every 664 years (242,547 days; semi-major axis of 76.11 AU). Its orbit has a moderate eccentricity of 0.32 and an inclination of 30° with respect to the ecliptic. The object belongs to the same orbital group as ("Buffy"), , and (also see diagram).
There is a special meaning of the expression "equinox (and ecliptic/equator) of date". When coordinates are expressed as polynomials in time relative to a reference frame defined in this way, that means the values obtained for the coordinates in respect of any interval t after the stated epoch, are in terms of the coordinate system of the same date as the obtained values themselves, i.e.
Explorer 35 (IMP-E, AIMP 2, Anchored IMP 2, Interplanetary Monitoring Platform-E) was a spin-stabilized spacecraft instrumented for interplanetary studies, at lunar distances, of the interplanetary plasma, magnetic field, energetic particles, and solar X rays. It was launched into an elliptical lunar orbit. The spin axis direction was nearly perpendicular to the ecliptic plane, and the spin rate was 25.6 rpm. Mission objectives were achieved.
Such occultations occur when the Moon's ascending node is near the autumnal equinox. A series of 49 occultations occurred starting on 29 January 2015 and ending at 3 September 2018. Each event was visible from points in the northern hemisphere or close to the equator; people in e.g. Australia or South Africa can never observe an Aldebaran occultation since it is too far south of the ecliptic.
Canterbury orbits the Sun in the central main-belt at a distance of 2.3–3.3 AU once every 4 years and 8 months (1,703 days). Its orbit has an eccentricity of 0.18 and an inclination of 7° with respect to the ecliptic. The asteroid was first identified as at Palomar Observatory, extending the body's observation arc by 7 years prior to its official discovery observation.
Hypsoma (Babylonian nisirti ašar or bit nisirti; "hidden place"; pl. hypsomata) is a Greek word indicating the Ecliptic high point of a celestial body, as seen from Earth (geocentric perspective). In Babylonian astronomy (wherein we have the prime mention of the phenomenon) the hypsomata of stars and planets are described in the Astrolabe B and in the mul.APIN: each star of Ea's path has its special hypsoma.
The tilt of the Earth's polar axis remains constant but describes a circular path in space during a period known as The Great Year. The term Great Year has two major meanings. It is defined by scientific astronomy as "The period of one complete cycle of the equinoxes around the ecliptic, or about 25,800 years". A more precise figure of 25,772 years is currently accepted.
Nikko orbits the Sun in the inner main-belt at a distance of 2.0–2.5 AU once every 3 years and 4 months (1,222 days). Its orbit has an eccentricity of 0.11 and an inclination of 6° with respect to the ecliptic. Nikkos observation arc begins with its first used observation taken at Johannesburg Observatory in 1930, or 3 years after its official discovery observation at Tokyo.
In addition, the ball itself is half white and half black and rotates around its own axis. From this information the lunar phases can be deduced: when the ball is all black, it is a new moon whereas an all white ball denotes a full moon. A metal circle divided into twelve decorated sections also rotates asymmetrically over the surface of the clock. It represents the ecliptic.
Lightcurve analysis indicates a somewhat angular shape and that Iris's pole points towards the ecliptic coordinates (β, λ) = (10°, 20°) with a 10° uncertainty. This gives an axial tilt of 85°, so that on almost a whole hemisphere of Iris, the sun does not set during summer, and does not rise during winter. On an airless body this gives rise to very large temperature differences.
Venetia orbits the Sun in the middle main-belt at a distance of 2.4–2.9 AU once every 4 years and 4 months (1,593 days). Its orbit has an eccentricity of 0.09 and an inclination of 10° with respect to the ecliptic. The body's observation arc begins in 1913, at the Collegio Romano Observatory () in Italy, approximately 17 months after its official discovery observation at Heidelberg.
Skuld is a member of the Flora family, one of the largest groups of stony S-type asteroids in the main-belt. It orbits the Sun in the inner main-belt at a distance of 1.8–2.7 AU once every 3 years and 4 months (1,215 days). Its orbit has an eccentricity of 0.20 and an inclination of 2° with respect to the ecliptic.
In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers, as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys . The study also determined two spin axes of (160.0°, 23.0°) and (353.0°, 24.0°) in ecliptic coordinates (λ, β).
Desdemona is a stony S-type asteroid that orbits the Sun in the middle main-belt at a distance of 2.0–3.2 AU once every 4 years and 2 months (1,525 days). Its orbit has an eccentricity of 0.24 and an inclination of 8° with respect to the ecliptic. As no precoveries were taken, the asteroid's observation arc begins with its official discovery observation at Heidelberg.
As it passed Jupiter, the probe fell through the planet's gravity field, exchanging momentum with the planet. The gravity assist maneuver bent the probe's trajectory northward relative to the Ecliptic Plane onto an orbit which passes over the poles of the Sun. By using this maneuver, Ulysses needed only enough propellant to send it to a point near Jupiter, which is well within current capability.
Itokawa belongs to the Apollo asteroids. They are Earth- crossing asteroids and the largest dynamical group of near-Earth objects with nearly 10,000 known members. Itokawa orbits the Sun at a distance of 0.95–1.70 AU once every 18 months (557 days; semi-major axis of 1.32 AU). Its orbit has an eccentricity of 0.28 and an inclination of 2° with respect to the ecliptic.
The star or star system is almost eclipsed by the sun on about 3 February, when it will figure behind the sun's corona if there is a full solar eclipse.In the Sky Earth astronomy reference utility showing the ecliptic and relevant date as at J2000 - present Thus the star can be viewed the whole night, crossing the sky, in early August (in the current epoch).
The asteroid is a member of the Koronis family, a collisional group consisting of a few hundred known bodies with nearly ecliptical orbits. It orbits the Sun in the outer main-belt at a distance of 2.6–3.0 AU once every 4 years and 9 months (1,747 days). Its orbit has an eccentricity of 0.07 and an inclination of 3° with respect to the ecliptic.
The S-type asteroid is a member of the Flora family, one of the largest groups of stony asteroids in the main- belt. It orbits the Sun in the inner main-belt at a distance of 2.0–2.4 AU once every 3 years and 2 months (1,161 days). Its orbit has an eccentricity of 0.09 and an inclination of 2° with respect to the ecliptic.
It orbits the Sun at a distance of 0.5–0.8 AU once every 6 months (186 days; semi-major axis of 0.64 AU). Its orbit has an eccentricity of 0.25 and a relatively high inclination of 33° with respect to the ecliptic. The orbital evolution of indicates that it is comfortably entrenched within the Atira orbital realm, but it might have arrived there relatively recently.
Stephania is a non-family asteroid of the main belt's background population, when applying the Hierarchical Clustering Method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 1.7–3.0 AU once every 3 years and 7 months (1,315 days). Its orbit has an eccentricity of 0.26 and an inclination of 8° with respect to the ecliptic.
Since it is near the ecliptic, Nu Scorpii can be occulted by the Moon and, very rarely, by planets. Mercury occulted it on 14 December 1821, but will not occult it again until 2 December 2031. The last occultation by Venus took place on 27 December 1852 and the next will take place on 30 December 2095. On 29 July 1808 there was an occultation by Neptune.
Accessed on line November 23, 2010. Together with Alpha Andromedae (Alpheratz) and Gamma Pegasi (Algenib), Beta Cassiopeiae was one of three bright stars known as the "Three Guides" marking the equinoctial colure. This is an imaginary line running due south from Beta Cassiopeiae through Alpha Andromedae to the celestial equator, at a point where the Sun's path (the ecliptic) crosses it each autumn and spring equinox.
Sárneczky is non-family asteroid from the main-belt's background population. It orbits the Sun in the outer asteroid belt at a distance of 2.9–3.5 AU once every 5 years and 7 months (2,053 days). Its orbit has an eccentricity of 0.09 and an inclination of 14° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Konkoly in 1940.
Cuppy orbits the Sun in the inner main-belt at a distance of 2.0–2.7 AU once every 3 years and 7 months (1,296 days). Its orbit has an eccentricity of 0.16 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins 7 years prior to its official discovery observation, with a precovery taken at Palomar Observatory in October 1991.
'Scorpio (') is the eighth astrological sign in the Zodiac, originating from the constellation of Scorpius. It spans 210°–240° ecliptic longitude. Under the tropical zodiac (most commonly used in Western astrology), the Sun transits this sign on average from October 23 to November 22. Under the sidereal zodiac (most commonly used in Hindu astrology), the Sun is in Scorpio from approximately November 16 to December 15.
Daléra orbits the Sun in the inner main-belt at a distance of 2.1–2.6 AU once every 3 years and 7 months (1,323 days). Its orbit has an eccentricity of 0.11 and an inclination of 4° with respect to the ecliptic. It was first identified as at Heidelberg Observatory in 1928, extending the body's observation arc by 11 years prior to its official discovery observation.
Dvořák is a Mars-crossing asteroid, as it crosses the orbit of Mars at 1.666 AU. It orbits the Sun at a distance of 1.6–3.0 AU once every 3 years and 6 months (1,283 days). Its orbit has an eccentricity of 0.31 and an inclination of 21° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Bergedorf in 1974.
Erbisbühl orbits the Sun in the inner main-belt at a distance of 1.5–3.2 AU once every 3 years and 7 months (1,324 days). Its orbit has an eccentricity of 0.38 and an inclination of 21° with respect to the ecliptic. The body's observation arc starts in 1963, as no precoveries were taken and no identifications were made prior to its official discovery.
Theta Aquarii (θ Aquarii, abbreviated Theta Aqr, θ Aqr), officially named Ancha (distinguish Ankaa, with the same pronunciation), is a star in the equatorial constellation of Aquarius. Visible to the naked eye at apparent magnitude 4.175, it is located at a distance of around from the Sun. Since it is near the ecliptic it can be occulted by the Moon, or very rarely by planets.
In sidereal and tropical astrology (including sun sign astrology), a 12-sign zodiac is used based on dividing the ecliptic into 12 equal parts rather than the IAU constellation boundaries. That is, astrological signs do not correspond to the constellations which are their namesakes, particularly not in the case of the tropical system where the divisions are fixed relative to the equinox, moving relative to the constellations.
Günter orbits the Sun in the inner main-belt at a distance of 1.7–2.8 AU once every 3 years and 4 months (1,224 days). Its orbit has an eccentricity of 0.24 and an inclination of 5° with respect to the ecliptic. As no precoveries were taken and no prior identifications were made, the body's observation arc begins at Heidelberg, one night after its official discovery observation.
The S-type asteroid orbits the Sun in the inner main-belt at a distance of 1.8–2.9 AU once every 3 years and 8 months (1,329 days). Its orbit has an eccentricity of 0.23 and an inclination of 3° with respect to the ecliptic. It was first identified as at Crimea–Nauchnij in 1979, extending the asteroid's observation arc by 11 years prior to its discovery.
Floris-Jan orbits the Sun in the inner main-belt at a distance of 1.9–3.0 AU once every 3 years and 10 months (1,401 days). Its orbit has an eccentricity of 0.21 and an inclination of 6° with respect to the ecliptic. First identified as at Simeiz Observatory in 1926, the body's observation arc begins 3 days after its official discovery observation at Johannesburg in 1930.
Sun and planets at local apparent noon (Ecliptic in red, Sun and Mercury in yellow, Venus in white, Mars in red, Jupiter in yellow with red spot, Saturn in white with rings). Even if the Earth's orbit were circular, the perceived motion of the Sun along our celestial equator would still not be uniform. This is a consequence of the tilt of the Earth's rotational axis with respect to the plane of its orbit, or equivalently, the tilt of the ecliptic (the path the Sun appears to take in the celestial sphere) with respect to the celestial equator. The projection of this motion onto our celestial equator, along which "clock time" is measured, is a maximum at the solstices, when the yearly movement of the Sun is parallel to the equator (causing amplification of perceived speed) and yields mainly a change in right ascension.
The asteroid belt (showing eccentricities), with the asteroid belt in red and blue ("core" region in red) Most asteroids within the asteroid belt have orbital eccentricities of less than 0.4, and an inclination of less than 30°. The orbital distribution of the asteroids reaches a maximum at an eccentricity of around 0.07 and an inclination below 4°. Thus although a typical asteroid has a relatively circular orbit and lies near the plane of the ecliptic, some asteroid orbits can be highly eccentric or travel well outside the ecliptic plane. Sometimes, the term main belt is used to refer only to the more compact "core" region where the greatest concentration of bodies is found. This lies between the strong 4:1 and 2:1 Kirkwood gaps at 2.06 and 3.27 AU, and at orbital eccentricities less than roughly 0.33, along with orbital inclinations below about 20°.
Gods are held to be immortal beings, who are human-like and yet invisible to human eyes. They are potencies who guide the development of the universe. The four main divine beings are: ① the universal supreme An/Dingir (literally "Heaven" or "Sky", astrally identified as the north ecliptic pole encompassed by the coil of the constellation Draco, and with all the constellations spinning around it; the Little Bear is his chariot, MULMar.gid.da.an.na, the "STARChariot of Heaven"), which is in turn identified as ② Ki or Ninhursag (; literally "Earth" or "Lady of the Mountains and Valleys"); ③ Enlil (; literally "Lord of the Breath", the god of weather and thunder, identified as MULApin, the "STARPlough", that is the constellation Triangulum, and generally with the northern sky—called Path of Enlil—, that is to say the circle nearest to the north ecliptic pole An; his wife Ninlil , literally "Lady of the Breath", is MULMar.gid.
' is located in the Lagrangian point, 60° behind Jupiter in the so-called Trojan camp. It is also a non-family asteroid of the Jovian background population. It orbits the Sun at a distance of 4.5–5.8 AU once every 11 years and 8 months (4,247 days; semi-major axis of 5.13 AU). Its orbit has an eccentricity of 0.12 and an inclination of 16° with respect to the ecliptic.
Rho Leonis (ρ Leo) is a binary star in the zodiac constellation of Leo, and, like the prominent nearby star Regulus, is near the ecliptic. With an apparent visual magnitude of 3.9, this star can be readily seen with the naked eye. Parallax measurements give a distance estimate of about from the Earth. This is an enormous star with about 21 times the Sun's mass () and 37 times the Sun's radius.
Either way, this suggests a loose rubble pile structure. Sylvia is also a fairly fast rotator, turning about its axis every 5.18 hours (giving an equatorial rotation velocity of about 230 km/h or 145 mph). The short axis is the rotation axis. Direct images indicate that Sylvia's pole points towards ecliptic coordinates (β, λ) = (+62.6°, 72.4°) with only a 0.5° uncertainty, which gives it an axial tilt of around 29.1°.
Al-Biruni orbits the Sun in the outer main-belt at a distance of 2.5–3.7 AU once every 5 years and 5 months (1,976 days). Its orbit has an eccentricity of 0.19 and an inclination of 15° with respect to the ecliptic. It was first identified as at Crimea- Nauchnij in 1981, extending the body's observation arc by 5 years prior to its official discovery at Rozhen.
Erato (minor planet designation: 62 Erato) is a carbonaceous Themistian asteroid from the outer region of the asteroid belt, approximately in diameter. Photometric measurements during 2004–2005 showed a rotation period of with an amplitude of in magnitude. It is orbiting the Sun with a period of , a semimajor axis of , and eccentricity of 0.178. The orbital plane is inclined by an angle of 2.22° to the plane of the ecliptic.
It has a 2:1 commensurability with Mars, having an orbital period double that of the planet. The orbital plane lies at an inclination of 6.0° to the plane of the ecliptic. This is a stony S-type asteroid with a cross-sectional size of 61 km, Photometry from the Oakley Observatory during 2006 produced a lightcurve that indicated a sidereal rotation period of with an amplitude of in magnitude.
Móra orbits the Sun in the inner main-belt at a distance of 2.3–2.7 AU once every 3 years and 11 months (1,434 days). Its orbit has an eccentricity of 0.08 and an inclination of 4° with respect to the ecliptic. Identified as , it was first observed at Heidelberg and Algiers Observatory in 1928, extending the body's observation arc by 4 years prior to its official discovery observation.
Mellena is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 2.1–3.3 AU once every 4 years and 5 months (1,610 days; semi- major axis of 2.69 AU). Its orbit has an eccentricity of 0.22 and an inclination of 8° with respect to the ecliptic.
Newcombia is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner main-belt at a distance of 1.9–2.8 AU once every 3 years and 8 months (1,326 days; semi-major axis of 2.36 AU). Its orbit has an eccentricity of 0.18 and an inclination of 11° with respect to the ecliptic.
The star is drifting further from the Earth with a heliocentric radial velocity of +15.2 km/s. It is located near the ecliptic and thus is subject to lunar occultations. This is an aging giant/bright giant star with a stellar classification of G8II-III, and is most likely (97% chance) on the horizontal branch. It is around 350 million years old with 3.3 times the mass of the Sun.
Whittemora is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.4–3.9 AU once every 5 years and 8 months (2,061 days; semi-major axis of 3.17 AU). Its orbit has an eccentricity of 0.23 and an inclination of 11° with respect to the ecliptic.
The carbonaceous asteroid is classified as a CU-type on the Tholen taxonomic scheme. It orbits the Sun at a distance of 1.9–3.0 AU once every 3 years and 10 months (1,407 days). Its orbit has an eccentricity of 0.21 and an inclination of 25° with respect to the ecliptic. Measurements using the adaptive optics at the W. M. Keck Observatory give a diameter estimate of 76 km.
In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys . The study also determined two spin axes of (238.0°, −15.0°) and (47.0°, −35.0°) in ecliptic coordinates (λ, β).
Ulla is the parent body of the Ulla family (), a very small asteroid family of less than 30 known bodies. It orbits the Sun in the outermost asteroid belt at a distance of 3.2–3.9 AU once every 6 years and 8 months (2,435 days; semi-major axis of 3.54 AU). Its orbit has an eccentricity of 0.09 and an inclination of 19° with respect to the ecliptic.
Romilda is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.6–3.7 AU once every 5 years and 8 months (2,057 days; semi-major axis of 3.17 AU). Its orbit has an eccentricity of 0.17 and an inclination of 11° with respect to the ecliptic.
Morishita is a S-type asteroid that orbits the Sun in the central main-belt at a distance of 2.0–3.2 AU once every 4 years and 2 months (1,508 days). Its orbit has an eccentricity of 0.22 and an inclination of 2° with respect to the ecliptic. As no precoveries were taken, and no prior identifications were made, the body's observation arc begins with its official discovery observation.
Plot of the Messier objects relative to the modern constellations, ecliptic, and Milky Way, using equatorial coordinates (right ascension, declination) A Messier marathon is an attempt, usually organized by amateur astronomers, to find as many Messier objects as possible during one night. The Messier catalogue was compiled by French astronomer Charles Messier during the late 18th century and consists of 110 relatively bright deep-sky objects (galaxies, nebulae, and star clusters).
Syringa is a non-family asteroid from the main belt's background population. It orbits the Sun in the intermediate asteroid belt at a distance of 1.7–3.5 AU once every 4 years and 3 months (1,558 days; semi- major axis of 2.63 AU). Its orbit has an eccentricity of 0.34 and an inclination of 6° with respect to the ecliptic. For a main-belt asteroid, it has a rather high eccentricity.
It orbits the Sun in the central main-belt at a distance of 2.1–3.4 AU once every 4 years and 8 months (1,693 days). Its orbit has an eccentricity of 0.24 and an inclination of 10° with respect to the ecliptic. It was first observed as at Heidelberg Observatory in 1901, extending the body's observation arc by 28 years prior to its official discovery observation at Barcelona.
Ptah orbits the Sun at a distance of 0.8–2.5 AU once every 2 years and 1 month (764 days). Its orbit has an eccentricity of 0.50 and an inclination of 7° with respect to the ecliptic. As no precoveries were taken, the asteroid's observation arc begins with its official discovery observation at Palomar. The potentially hazardous asteroid has a minimum orbit intersection distance with Earth of or 10 lunar distances.
Several lightcurve were also modeled from the abundant photometric observations. In 1994 and 1995, Polish astronomers obtained a concurring period 5.223328 hours and found a spin axis of (54.0°, −52.0°) in ecliptic coordinates (λ, β) (). Radiometric observations gave a period of 5.223327 hours and a pole of (55.0°, −46.0°). Two other international studies obtained a period of 5.223326 hours and a pole at (56.0°, −47.0°) and (55.0°, −45.0°), respectively ().
Bogoslovskij orbits the Sun in the central main-belt at a distance of 2.3–3.2 AU once every 4 years and 6 months (1,658 days). Its orbit has an eccentricity of 0.16 and an inclination of 14° with respect to the ecliptic. In the SMASS classification, Bogoslovskij is an uncommon Cgh-type, which belongs to the broader class of carbonaceous asteroids. As of 2017, no rotational lightcurve has been obtained.
Bonsdorffia is a non-family asteroid of the main belt's background population. It orbits the Sun in the outer main-belt at a distance of 2.3–4.1 AU once every 5 years and 9 months (2,090 days). Its orbit has an eccentricity of 0.28 and an inclination of 16° with respect to the ecliptic. The body's observation arc begins 11 days prior to its official discovery observation at Turku.
Boreas orbits the Sun at a distance of 1.3–3.3 AU once every 3 years and 5 months (1,251 days). Its orbit has an eccentricity of 0.45 and an inclination of 13° with respect to the ecliptic. The near-Earth asteroid has an Earth minimum orbit intersection distance of , which corresponds to 98.2 lunar distances. Its observation arc begins with it official discovery observation at Uccle in 1953.
Boyer is a member of the Eunomia family (), the most prominent family in the intermediate main-belt, which mostly consists of stony asteroids. Conversely, Boyer has also been grouped into the Maria family (). It orbits the Sun at a distance of 2.2–2.9 AU once every 4 years and 2 months (1,512 days). Its orbit has an eccentricity of 0.13 and an inclination of 16° with respect to the ecliptic.
Records is a non-family from the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 1.9–3.6 AU once every 4 years and 7 months (1,679 days). Its orbit has an eccentricity of 0.32 and an inclination of 5° with respect to the ecliptic. As no precoveries were taken, the body's observation arc begins with its official discovery observation in 1955.
In May 2002, a rotational lightcurve of Jeanne was obtained from photometric observations by French amateur astronomer Christophe Demeautis. Lightcurve analysis gave a rotation period of 15.18 hours with a brightness amplitude of 0.45 magnitude (). A lightcurve was also modeled using photometric data from the Lowell Photometric Database. It gave a concurring sidereal period of hours and two spin axes at (153.0°, 19°) and (338.0°, 32.0°) in ecliptic coordinates (λ, β).
Ulysses' second orbit: it arrived at Jupiter on February 8, 1992, for a swing-by maneuver that increased its inclination to the ecliptic by 80.2 degrees. Usually observational astronomy is considered to occur on Earth's surface (or beneath it in neutrino astronomy). The idea of limiting observation to Earth includes orbiting the Earth. As soon as the observer leaves the cozy confines of Earth, the observer becomes a deep space explorer.
Ishtar orbits the Sun at a distance of 1.2–2.8 AU once every 2 years and 9 months (1,018 days; semi-major axis of 1.98 AU). Its orbit has an eccentricity of 0.39 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with its first observation at the Siding Spring Observatory in March 1981, almost 11 years prior to its official discovery observation at Palomar.
Hedera is a non-family asteroid from the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.3–3.1 AU once every 4 years and 6 months (1,636 days; semi-major axis of 2.72 AU). Its orbit has an eccentricity of 0.16 and an inclination of 6° with respect to the ecliptic. The asteroid was first observed as at Heidelberg in April 1907.
Fukushima orbits the Sun in the inner main-belt at a distance of 2.3–2.5 AU once every 3 years and 10 months (1,392 days). Its orbit has an eccentricity of 0.04 and an inclination of 14° with respect to the ecliptic. The asteroid was first identified as at Heidelberg Observatory in 1926, extending the body's observation arc by 62 years prior to its official discovery observation at Kitami.
Geisei is a member of the Flora family, one of the largest families of stony asteroids. It orbits the Sun in the inner main-belt at a distance of 1.8–2.7 AU once every 3 years and 4 months (1,215 days). Its orbit has an eccentricity of 0.19 and an inclination of 3° with respect to the ecliptic. In October 1911, Geisei was first identified as at Heidelberg Observatory.
Guinevere orbits the Sun at a distance of 2.9–5.1 AU once every 7 years and 11 months (2,890 days). Its orbit has an eccentricity of 0.28 and an inclination of 5° with respect to the ecliptic. In November 1921, it was first identified as at Bergedorf Observatory in Hamburg, Germany. The body's observation arc begins two nights after its official discovery observation at Heidelberg in August 1928.
Ilona orbits the Sun in the inner main-belt at a distance of 2.0–2.5 AU once every 3 years and 5 months (1,241 days). Its orbit has an eccentricity of 0.12 and an inclination of 9° with respect to the ecliptic. The asteroid was first identified as at Bergedorf Observatory in September 1915. The body's observation arc, however, begins at Heidelberg one night after its official discovery observation.
Inanda is a non-family asteroid of the main belt's background population. It orbits the Sun in the central main-belt at a distance of 1.9–3.2 AU once every 4 years and 1 month (1,479 days; semi-major axis of 2.54 AU). Its orbit has an eccentricity of 0.26 and an inclination of 7° with respect to the ecliptic. The asteroid was first identified as at Johannesburg in September 1926.
Gorizia orbits the Sun in the inner main-belt at a distance of 2.2–2.6 AU once every 3 years and 9 months (1,371 days). Its orbit has an eccentricity of 0.09 and an inclination of 5° with respect to the ecliptic. In 1976, it was first identified as at the Japanese Kiso Observatory, extending the body's observation arc by 19 years prior to its official discovery observation.
Felixhormuth is a non-family asteroid from the main belt's background population. It orbits the Sun in the outer main-belt at a distance of 2.7–3.6 AU once every 5 years and 7 months (2,047 days). Its orbit has an eccentricity of 0.14 and an inclination of 7° with respect to the ecliptic. The body's observation arc begins at Palomar with its official discovery observation in March 1971.
However, a different HCM-based analysis assigns Deiphobus to the Jovian background population. It orbits the Sun at a distance of 4.9–5.4 AU once every 11 years and 7 months (4,241 days; semi-major axis of 5.13 AU). Its orbit has an eccentricity of 0.04 and an inclination of 27° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Leoncito in March 1971.
Elysiasegal orbits the Sun in the inner main-belt at a distance of 2.0–2.8 AU once every 3 years and 8 months (1,351 days). Its orbit has an eccentricity of 0.17 and an inclination of 2° with respect to the ecliptic. A first precovery was taken by the Near-Earth Asteroid Tracking program in 1996, extending the asteroid's observation arc by 2 years prior to its official discovery observation.
Ariane orbits the Sun at a distance of 2.1–2.4 AU once every 3 years and 4 months (1,219 days). Its orbit has an eccentricity of 0.07 and an inclination of 3° with respect to the ecliptic. Photometric observations made in 2003 at the U.S. Carbuncle Hill Observatory (912) near Providence, Rhode Island, give a synodic rotation period of hours. The light curve shows a brightness variation of in magnitude.
Ankara orbits the Sun in the middle of the main-belt at a distance of 2.3–3.1 AU once every 4 years and 5 months (1,618 days). Its orbit has an eccentricity of 0.15 and an inclination of 6° with respect to the ecliptic. It was first observed as at Uccle Observatory in 1933, extending the body's observation arc by 4 years prior to its official discovery observation at Heidelberg.

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