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230 Sentences With "most luminous"

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

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It's afraid of the dark, and that's where Wilder is most luminous.
A team of scientists may have found the most luminous supernova yet discovered.
Despite their name, supermassive black holes are among the most luminous objects in the universe.
This production is afraid of the dark, and that's where Wilder is most luminous (1:30).
As a paradoxical result, supermassive black holes can be the most luminous objects in the universe.
"London is not exactly the most luminous city, and it has a long winter," he said.
Locke would feed and discipline that spirit, playing the critic, publicist, taskmaster, and impresario to the movement's most luminous figures.
Michel Foucault's most luminous idea was that power and knowledge are mutually constituted social phenomena, and that they cannot be disentangled.
Quasars make up the centers of massive galaxies, and they're thought to be some of the most luminous objects in the Universe.
McConaughey impersonation is a competitive industry, with some of today's most luminous stars trying their hands at his Texas drawl and meandering philosophical tangents.
And it's in the desert wasteland of Gariseb, where Rebecca feverishly treats all comers, that McNeil's writing is most luminous, both spare and powerful.
All four shades in the just-launched Dior Backstage Glow Palette subtly enhance my skin, giving not just my cheekbones, but my entire face the most luminous glow.
" V. S. Pritchett, in a review of "Blindness," which was available for the first time since 1932, called Green "the most luminous novelist of the Thirties and Forties.
"This is not precisely the 'largest' supernova, but the most luminous yet seen," said Robert Kirshner, a supernova expert at Harvard University, who was not involved in the study.
Self-possessed and hugely popular, Johnson was probably the most luminous celebrity in the state of Montana from 2011 through 2014, when he led the Griz to many dramatic victories.
These "fast radio bursts," or FRBs, last just a few milliseconds, but they are the most luminous radio signals in the universe, powered by as much energy as 22004 million suns.
On July 15, 219, the designer Gianni Versace was gunned down on the steps of his Miami Beach mansion, leaving the fashion world to mourn one of its most luminous stars.
So whether you're looking for a lightweight gel that delivers the most luminous non-oily shine, or a bronzy glow that fakes a natural tan, you'll find your moisturizer, cheap and accessible, ahead.
This Sunday, basketball's most luminous talent will form an aurora borealis in Toronto at the 20063th NBA All-Star Game, with starting lineups that include Kobe Bryant, LeBron James, Stephen Curry, and Kevin Durant.
It's hard to imagine that toward the end of this century, it will be the most luminous star in the Milky Way galaxy when it explodes, according to Louisiana State University astronomer Bradley Schaefer.
The black hole in question (pictured below) is located at the centre of a galaxy 55m light-years from Earth called Messier 87, one of the largest and most luminous galaxies in the nearby universe.
But perhaps the most luminous part of her glam was her décolleté and legs, which were coated in her new Body Lava Body Luminizer in Brown Sugar and topped off with the Fairy Bomb Glittering Pom Pom.
This gluttonous spectacle, courtesy of NASA's space-based Wide-field Infrared Survey Explorer, captures not the biggest or grandest of galaxies, but one of the most luminous such bodies ever discovered—350 trillion times brighter than our sun.
This gluttonous spectacle, courtesy of NASA's space-based Wide-field Infrared Survey Explorer, captures not the biggest or grandest of galaxies, but one of the most luminous such bodies ever discovered—20183 trillion times brighter than our sun.
Eta Carinae is the most luminous and massive stellar system with 10,20103 light-years, and is best known for an enormous eruption in the 1840s that hurled at least 10 times the sun's mass into space, leaving an expanding veil of gas and dust.
A distance of 5 kpc and a bolometric magnitude of -9.4 put HR Car among the most luminous stars of the galaxy.
RS Puppis has one of the longest periods of Cepheids in the Milky Way and therefore is also one of the most luminous.
From the redshift of the lines Ulrich deduced that TON 618 was very distant, and hence was one of the most luminous quasars known.
WR 102ea is a Wolf–Rayet star in the Sagittarius constellation. It is the second most luminous star in the Quintuplet cluster after WR 102hb. With a luminosity of 2,500,000 times solar, it is also one of the most luminous stars known. Despite the high luminosity it can only be observed at infra-red wavelengths due to the dimming effect of intervening dust on visual light.
The pulsations of Alpha Cygni Variable stars are not fully understood. They are not confined to a narrow range of temperatures and luminosities in the way that most pulsating stars are. Instead, most luminous A and B supergiants, and possibly also O and F stars, show some type of unpredictable small-scale pulsations. Nonadiabatic strange mode radial pulsations are predicted but only for the most luminous supergiants.
There are no known supernova progenitors corresponding to the most luminous red supergiants, and it is expected that these evolve to Wolf Rayet stars before exploding.
It may have been perhaps the most luminous such events ever observed coming from a red dwarf star. A secondary radio flare was observed a day later.
3XMM J004232.1+411314 is a low-mass X-ray binary hosted in the galaxy M31. This object is notable for being the most luminous source of hard X-rays in the Andromeda Galaxy. This is also the most luminous source known that shows dips in the X-ray light curve. The compact object in this system has been unambiguously identified as a neutron star with a spin period of 3 seconds.
WR 102ka, also known as the Peony star, is a Wolf–Rayet star that is one of several candidates for the most luminous-known star in the Milky Way.
AE Andromedae (AE And) is a luminous blue variable (LBV), a type of variable star. The star is one of the most luminous variables in M31, the Andromeda Galaxy.
R145 (HD 269928) is a spectroscopic binary star in the Tarantula Nebula in the Large Magellanic Cloud located in the constellation Dorado. Both components are amongst the most luminous known.
PKS 2000-330 (also known as QSO B2000-330) is a quasar located in the constellation Sagittarius. When identified in 1982, it was the most distant and most luminous object known.
Zeta Puppis (ζ Puppis, abbreviated Zeta Pup, ζ Pup), formally named Naos , is a star in the constellation of Puppis. The spectral class of O4 means this is one of the hottest, and most luminous, stars visible to the naked eye. It is one of the sky's few naked-eye class O-type stars as well as one of the closest to Earth. It is a blue supergiant, one of the most luminous stars in the Milky Way.
H-R Diagram showing the location of the luminous blue variables and their typical behaviour during an outburst. R71 is one of the most luminous stars known, and the most luminous in the Magellanic Clouds during the 2012 outburst. During quiescence, it appears as like other very luminous early B supergiants, about 15,000 K and . The radius of this type of stars is not well-defined as it has a dense stellar wind and is losing mass at about every three million years.
A concise encyclopedia of the Baháʼí Faith. Oxford: Oneworld Publications. . He was the son of his father's second wife, Fatimih Khanum. His father gave him the title G͟husn-i-Anwar (“The Most Luminous Branch”).
Eventually, the cluster would be resolved and found to contain three of the most massive and most luminous stars known, as well as a number of luminous O class stars and many fainter stars.
R71 (RMC 71, HD 269006) is a star in the Large Magellanic Cloud (LMC) in the constellation Mensa. It is classified as a luminous blue variable and is one of the most luminous stars in the LMC.
HD 269810 is a blue giant star in the Large Magellanic Cloud. It is one of the most massive and most luminous stars known, and one of only a handful of stars with the spectral type O2.
BAT99-98 is a star in the Large Magellanic Cloud. It is located near the R136 cluster in the 30 Doradus nebula. At and it is the third most massive and the fifth most luminous star known.
He studied for his doctorate under Gerard de Vaucouleurs and Fritz Zwicky at the University of Texas at Austin, receiving his degree in 1970. Fairall discovered and named Fairall 9, the most luminous Seyfert 1 (active) galaxy.
LSS 4067 has an absolute bolometric magnitude of −11.4, making it one of the most luminous stars known. Indeed, many of the hottest and most luminous stars known are O-type supergiants, or Wolf-Rayet stars. LSS 4067 has an unusual spectrum, with various emission lines including N III and He II emission lines, thus the "f" in its spectral type. Because of this unusual spectrum, classifying the star or deducing its properties has proved relatively difficult: for example, the effective temperature is predicted to be too cool and the surface gravity too high.
Observations from the Palomar Transient Factory, reported in 2009, indicate a redshift z = 1.189 and a peak magnitude of −23.5 absolute (comparable to SN2005ap), making SCP 06F6 one of the most luminous transient phenomena known as of that date.
BI 253 is an O2V star in the Large Magellanic Cloud and is a primary standard of the O2 type. It is one of the hottest main-sequence stars known and one of the most-massive and most-luminous stars known.
The supergiant luminosity class is assigned on the basis of spectral features that are largely a measure of surface gravity, although such stars are also affected by other properties such as microturbulence. Supergiants typically have surface gravities of around log(g) 2.0 cgs and lower, although bright giants (luminosity class II) have statistically very similar surface gravities to normal Ib supergiants. Cool luminous supergiants have lower surface gravities, with the most luminous (and unstable) stars having log(g) around zero. Hotter supergiants, even the most luminous, have surface gravities around one, due to their higher masses and smaller radii.
AH Scorpii (abbreviated to AH Sco) is a red supergiant variable star located in the constellation Scorpius. It is one of the largest stars known by radius and is also one of the most luminous red supergiant stars in the Milky Way.
Supergiants are among the most massive and most luminous stars. Supergiant stars occupy the top region of the Hertzsprung–Russell diagram with absolute visual magnitudes between about −3 and −8. The temperature range of supergiant stars spans from about 3,400 K to over 20,000 K.
The telltale signs of the collision are two extended luminous tails swirling out from the galaxy. The tails are studded with a particularly high density of star clusters. NGC 3256 is the most luminous galaxy in the infrared spectrum located within z 0.01 from Earth.
NML Cygni or V1489 Cygni (abbreviated to NML Cyg or V1489 Cyg) is a red hypergiant or red supergiant (RSG) in the constellation Cygnus. It is one of the largest stars currently known by radius, and is also one of the most luminous and massive cool hypergiants, as well as one of the most luminous stars in the Milky Way. The distance of NML Cygni from Earth is estimated to be around 1.6 kpc, about . It is a part of the Cygnus OB2 association, one of the closest massive associations to the Sun, spanning nearly 2° on the sky or ∼ in radius at the distance of .
The presbytery is the most luminous area in the church. It is formed by the seventh bay of the nave, and includes the high altar. On the side walls are two further Fiamminghini works: Adoration of the Shepherds and the Madonna del Latte. Bernardino Luini's Madonna della Buonanotte.
For example, the giant elliptical galaxy M87 has an absolute magnitude of −22 (i.e. as bright as about 60,000 stars of magnitude −10). Some active galactic nuclei (quasars like CTA-102) can reach absolute magnitudes in excess of −32, making them the most luminous objects in the observable universe.
The nebula was named in the 1980s for its shape as seen in low resolution images that were available at the time. The Pistol Star, a luminous blue variable is 1.6 million times brighter than the Sun making it one of the most luminous stars in the Milky Way.
M82 X-1 is an ultra-luminous X-ray source located in the galaxy M82. It is a candidate intermediate-mass black hole, with the exact mass estimate varying from around 100 to 1000. One of the most luminous ULXs ever known, its mass goes over the Eddington limit.
Abell 2667 is a galaxy cluster. It is one of the most luminous galaxy clusters in the X-ray waveband known at a redshift about 0.2. This cluster is also a well-known gravitational lens. On 2 March 2007, a team of astronomers reported the detection of the Comet Galaxy in this cluster.
To date, this is the most luminous source that shows dips in its X-ray lightcurves. The compact object of this system is a neutron star with a spin period of 3 seconds, and this is proved by the observation of a modulation with the same period in the X-ray luminosity.
The nature of ASASSN-15lh is disputed. The most popular explanations are that it is the most luminous type I supernova (hypernova) ever observed, or a tidal disruption event around a supermassive black hole. Other hypotheses include: gravitational lensing; a quark nova inside a Wolf–Rayet star; or a rapid magnetar spindown.
Stars #28 and #105 are Wolf-Rayet stars. Star #27, a blue giant star with a spectral type of O8III((f)), may be one of the most luminous stars known, with a bolometric magnitude of −10.5. Star #102 is known as V925 Scorpii or HD 159378, and is a rare yellow supergiant star.
VY Canis Majoris (abbreviated to VY CMa) is an extreme oxygen-rich (O-rich) red hypergiant (RHG) or red supergiant (RSG) and pulsating variable star located at away from Earth in the constellation of Canis Major. It is one of the largest known stars by radius, and is also one of the most luminous and massive red supergiants, as well as one of the most luminous stars in the Milky Way. VY CMa is a single star with a large infrared (IR) excess, making it one of the brightest objects in the sky at wavelengths of between 5 and 20 microns (µm) and indicating a dust shell or disk heated by the star. It is about times the mass of the Sun ().
The brightest star is WR 25 WR 25 is a binary system in the central portion of the Carina Nebula, a member of the cluster. The primary is a Wolf–Rayet star, possibly the most luminous star in the galaxy. The secondary is hard to detect but thought to be a luminous OB star.
VFTS 682 is a Wolf–Rayet star in the Large Magellanic Cloud. It is located over north-east of the massive cluster R136 in the Tarantula Nebula. It is 150 times the mass of the sun and 3.2 million times more luminous which makes it one of the most massive and most luminous stars known.
BAT99-116 (commonly called Melnick 34 or Mk34) is a binary Wolf–Rayet star near R136 in the 30 Doradus complex (also known as the Tarantula Nebula) in the Large Magellanic Cloud. Both components are amongst the most massive and most luminous stars known, and the system is the most massive known binary system.
Despite being one of the most luminous stars in the Milky Way, much of the visible light of VY CMa is absorbed by the circumstellar envelope, so it cannot be seen with the naked eye and needs a telescope to be observed. It would be a naked eye star if no light was absorbed.
WR 22, also known as V429 Carinae or HR 4188, is an eclipsing binary star system in the constellation Carina. The system contains a Wolf-Rayet (WR) star that is one of the most massive and most luminous stars known, and is also a bright x-ray source due to colliding winds with a less massive O class companion.
Alpha Cygni, called Deneb, is the brightest star in Cygnus. It is a white supergiant star of spectral type A2Iae that varies between magnitudes 1.21 and 1.29, one of the largest and most luminous A-class stars known. It is located about 3200 light-years away. Its traditional name means "tail" and refers to its position in the constellation.
Pismis 24-1, also known as HD 319718, is the brightest star of the open cluster Pismis 24 within the nebula NGC 6357 about 6,500 light-years away. It was once thought to be the most massive star known, but is composed of at least three individual objects, each still among the most luminous and most massive stars known.
If a black hole spins slowly, it will not repel its gas absorption as much. A slow- spinning black hole can absorb more matter than a fast-spinning black hole. The massive black holes in ELIRGs could be absorbing matter for a longer time. Twenty new ELIRGs, including the most luminous galaxy found to date, have been discovered.
It has been described as similar to the Sextans Dwarf Galaxy. Both galaxies are ancient and metal- deficient. It estimated to be located at a distance of about 330,000 light- years (100 kpc) from the Earth. That is about twice the distance to the Large Magellanic Cloud; the largest and most luminous satellite galaxy of the Milky Way.
R136b is a Wolf-Rayet star in the R136 cluster in the Large Magellanic Cloud. It is one of the most massive and most luminous stars known. It is found in the dense R136 open cluster at the centre of NGC 2070 in the Tarantula Nebula. R136b has the spectral type of Wolf-Rayet star, with strong emission lines.
BX Andromedae, like all Beta Lyrae variables, shows a primary and a secondary minimum when, respectively, the most luminous and the less luminous component of the pair is eclipsed by the other. The brightness however changes smoothly, so there is no onset and an end time for the eclipses. This cycle repeats approximately every 14.6 hours.
Trumpler 16 (Tr 16) is a massive open cluster that is home to some of the most luminous stars in the Milky Way galaxy. It is situated within the Carina Nebula complex in the Carina–Sagittarius Arm, located approximately from Earth. The cluster has one star visible to the naked eye from the tropics southward, Eta Carinae.
Recent estimates place it somewhat nearer to Earth, which when combined with its binary nature mean that it is now well within the expected range of parameters for extremely luminous stars in the galaxy. It is estimated at 2 million times as luminous as the sun which makes it one of the most luminous stars in the galaxy.
WR 12 (V378 Velorum) is a spectroscopic binary in the constellation Vela. It is an eclipsing binary consisting of a Wolf-Rayet star and a luminous companion of unknown spectral type. The primary is one of the most luminous stars known. The spectrum of WR 12 is dominated by the broad emission lines of the primary Wolf-Rayet star.
Rho Cassiopeiae is a semi-regular pulsating variable yellow hypergiant, among the most luminous stars in the galaxy at approximately . It has a minimum magnitude of 6.2 and a maximum magnitude of 4.1; its period is approximately 320 days. It has around 450 times the Sun's diameter and 17 times its mass, having begun life 45 times as massive as the Sun.
Also known as the S Doradus variables, the most luminous stars known belong to this class. Examples include the hypergiants η Carinae and P Cygni. They have permanent high mass loss, but at intervals of years internal pulsations cause the star to exceed its Eddington limit and the mass loss increases hugely. Visual brightness increases although the overall luminosity is largely unchanged.
P Cygni (34 Cyg) is a variable star in the constellation Cygnus. The designation "P" was originally assigned by Johann Bayer in Uranometria as a nova. Located about 5,000 to 6,000 light-years (1,500–1,800 parsecs) from Earth, it is a hypergiant luminous blue variable (LBV) star of spectral type B1Ia+ that is one of the most luminous stars in the Milky Way.
Examples of core-collapsed globular clusters include M15 and M30. 47 Tucanae – the second most luminous globular cluster in the Milky Way, after Omega Centauri. Core-collapse is thought to occur when the more massive stars in a globular cluster encounter their less massive companions. Over time, dynamic processes cause individual stars to migrate from the center of the cluster to the outside.
The primary, slightly hotter, star is observed to be the less massive of the two. Each star is amongst the most luminous known, but the exact parameters of each has not been determined. Their combined luminosity is around to . The masses have not yet been calculated accurately from the orbital parameters, but the stars have been modelled to initially have been around and .
Chandra image of the core of NGC 4636 with superimposed contours of Hα+[N ii] emission. White crosses mark the detected CO cloud positions. NGC 4636 is one of the most luminous nearby elliptical galaxies when observed in X-rays, with estimated X-ray flux of erg/s. A hot gas corona around the galaxy was first detected by the Einstein Observatory.
Seven of the globular clusters have X-ray counterparts, which are among the most luminous X-ray sources in NGC 5846. These clusters are mostly in the central region and they are optically luminous, compact and belong to the red subpopulation. Chandra image of NGC 5846 with superimposed contours of Hα+[N ii] emission. White crosses mark the detected CO cloud positions.
AG Carinae (AG Car) is a star in the constellation Carina. It is classified as a luminous blue variable and is one of the most luminous stars in the Milky Way. The large distance (20,000 light-years) and intervening dust mean that the star is not usually visible to the naked eye; its apparent brightness varies erratically between magnitude 5.7 and 9.0.
Hyper luminous Infrared Galaxies (HyLIRG), also referred to as HiLIRGs and HLIRGs, are considered to be some of the most luminous persistent objects in the Universe, exhibiting extremely high star formation rates, and most of which are known to harbour Active Galactic Nuclei (AGN). They are defined as galaxies with luminosities above 1013 L⊙, as distinct from the less luminous population of ULIRGs (L = 1012 – 1013 L⊙). HLIRGs were first identified through follow-up observations of the IRAS mission. IRAS F10214+4724, a HyLIRG being gravitationally lensed by a foreground elliptical galaxy, was considered to be one of the most luminous objects in the Universe having an intrinsic luminosity of ~ 2 × 1013 L⊙. It is believed that the bolometric luminosity of this HLIRG is likely amplified by a factor of ~30 as a result of the gravitational lensing.
HD 93129 is a triple star system of O-class stars in Carina. All three stars of are among the most luminous in the galaxy; consists of two clearly resolved components, and , and itself is made up of two much closer stars. HD 93129 A has been resolved into two components. The spectrum is dominated by the brighter component, although the secondary is only 0.9 magnitudes fainter.
Red supergiants are the largest type of star, but the most luminous are much smaller and hotter, with temperatures up to 50,000 K and more and luminosities of several million L⊙, meaning their radii are just a few tens of R⊙. For example, R136a1 has a temperature over 50,000 K and a luminosity of more than 8,000,000 L⊙ (mostly in the UV), it is only .
A second candidate was announced in 2011. Messier 49 was the first member of the Virgo Cluster of galaxies to be discovered. It is the most luminous member of that cluster and more luminous than any galaxy closer to the Earth. This galaxy forms part of the smaller Virgo B subcluster located 4.5° away from the dynamic center of the Virgo Cluster, centered on Messier 87.
The brightness temperature of a pulse with such high flux density and such low duration exceeds 5 kelvins, making the pulses of PSR B1937+21 the brightest radio emission ever observed. PSR B1937+21 is intrinsically the most luminous millisecond pulsar. In addition to the radio pulses observed, pulses have been detected at x-ray wavelengths, which show the same pulse and interpulse pattern.
It has an apparent magnitude of 10.3. Within it lies the triple star system HD 5980, each of its members among the most luminous stars known. Open star cluster NGC 299 is located within the Small Magellanic Cloud. The Tucana Dwarf galaxy, which was discovered in 1990, is a dwarf spheroidal galaxy of type dE5 that is an isolated member of the Local Group.
These regions are associated with molecular clouds containing solar masses. The brightest of these regions, NGC 604, may have undergone a discrete outburst of star formation about three million years ago. This nebula is the second most luminous HII region within the Local Group of galaxies, at times the luminosity of the Sun. Other prominent HII regions in Triangulum include IC 132, IC 133, and IK 53.
M33-013406.63, also known as B416, is a blue supergiant star in the constellation of Triangulum. It is located within the Triangulum Galaxy, which is approximately 2,380,000–3,070,000 light years away from Earth. It is the most luminous star ever discovered and one of the largest stars in the Triangulum Galaxy. It is estimated to be approximately 6,400,000–10,280,000 times more luminous than the Sun.
Its emission appears elongated at a position angle perpendicular to the dust lane, with the most luminous region being in the nucleus. The emission extends for more than 5 arcminutes in 610 MHz. In 1.4 GHz, the galaxy has one jet with FRI morphology, that extends for more than 3 kpc. In 5 GHz, emission appears in the nucleus and two jet-like structures.
P. Goode and colleagues at Big Bear Solar Observatory have measured the earthshine and T. Livengood of NASA analyzed the EPOXI data. Earth as seen from Venus near opposition from the Sun would be extremely bright at magnitude −6. To an observer outside the Earth's orbit on Mars our planet would appear most luminous near the time of its greatest elongation from the Sun, at about magnitude −1.5.
V4650 Sgr is calculated to be one of the most luminous stars known, at to . It is considered to be a bona-fide luminous blue variable, although it has not been observed to change temperature from the S Doradus minimum strip to a cooler outburst state. The infrared brightness has varied between magnitude 7.0 and 7.9. It is calculated to have a temperature of 11,300 K and a radius of .
Located 4 degrees south of Sirius, it contains contrasting blue, yellow and orange stars and covers an area the apparent size of the full moon—in reality around 25 light-years in diameter. Its most luminous stars have already evolved into giants. The brightest is a 6.3-magnitude star of spectral type K3. Located in the field is 12 Canis Majoris, though this star is only 670 light-years distant.
BI 253 is one of the hottest, most massive, and most luminous known main sequence stars. The temperature is around 50,000 K, the luminosity over , and the mass over , although it is less than . The rotation rate of at least 200 km/s is high, but this is common in the youngest and hottest stars, either due to spin-up during stellar formation or merger of a close binary system.
The Pistol Star is an extremely luminous blue hypergiant star; one of the most luminous and massive known in the Milky Way. It is one of many massive young stars in the Quintuplet cluster in the Galactic Center region. The star owes its name to the shape of the Pistol Nebula, which it illuminates. It is located approximately 25,000 light years from Earth in the direction of Sagittarius.
Deneb () is a first-magnitude star in the constellation of Cygnus, the swan. Deneb is one of the vertices of the asterism known as the Summer Triangle and the "head" of the Northern Cross. It is the brightest star in Cygnus and the 19th brightest star in the night sky, with an average apparent magnitude of +1.25. A blue-white supergiant, Deneb rivals Rigel as the most luminous first magnitude star.
Each area of the sky was scanned at least 10 times at the equator; the poles were scanned at theoretically every revolution due to the overlapping of the images. The produced image library contains data on the local Solar System, the Milky Way, and the more distant universe. Among the objects WISE studied are asteroids, cool, dim stars such as brown dwarfs, and the most luminous infrared galaxies.
HR Carinae is a luminous blue variable star located in the constellation Carina. It is surrounded by a vast nebula of ejected nuclear-processed material because this star has a multiple shell expanding atmosphere. This star is among the most luminous stars in the Milky Way. It has very broad emission wings on the Balmer lines, reminiscent from the broad lines observed in the spectra of O and Wolf–Rayet stars.
Westerlund 1-237 or Wd 1-237 is a possible red supergiant (RSG) in the constellation of Ara. It is one out of 4 known red supergiants in the Westerlund 1 super star cluster, although its outlying position, spectrum, and parallax, suggest it could be a foreground giant. As a red supergiant, it would be one of the largest known stars and one of most luminous of its type.
R136c is a star located in R136, a tight knot of stars at the centre of NGC 2070, an open cluster weighing 450,000 solar masses and containing 10,000 stars. At and 5.6 million , it is the most massive star known and one of the most luminous, along with being one of the hottest, at 51,000 K. It was first resolved and named by Feitzinger in 1980, along with R136a and R136b.
R136a3 is a Wolf–Rayet star in R136, a massive star cluster located in Dorado. It is located near R136a1, the most massive and luminous star known. R136a3 is itself one of the most massive and most luminous stars known at 180 times more massive and 3.8 million times more luminous than the Sun. The formal name of the star is RMC 136a3, standing for Radcliffe observatory, Magellanic Clouds, 136a3.
WR 24 (HD 93131) is a Wolf-Rayet star in the constellation Carina. It is one of the most luminous stars known. At the edge of naked eye visibility it is also one of the brightest Wolf Rayet stars in the sky. The spectrum of WR 24 has the characteristic strong nitrogen and helium emission lines of a WN star, but also lines of hydrogen that show Doppler-displaced absorption components.
WR 148 is a spectroscopic binary in the constellation Cygnus. The primary star is a Wolf-Rayet star and one of the most luminous stars known. The secondary has been suspected of being a stellar-mass black hole but may be a class O main sequence star. WR 148 shows a classic WN8h spectrum, but with the addition of weak central absorption on some of the emission lines.
Quintuplet cluster region, centred on the Pistol nebula The Pistol Nebula is located in the constellation Sagittarius. It surrounds one of the most luminous stars known, the Pistol Star. Both are located 25,000 light years away from Earth in the Quintuplet cluster, near the center of the Milky Way galaxy. The nebula contains approximately 9.3 solar masses worth of ionized gas that was ejected by the star several thousand years ago.
The Alpha Persei Cluster, also known as Melotte 20 or Collinder 39, is an open cluster of stars in the northern constellation of Perseus. To the naked eye, the cluster consists of several blue-hued spectral type B stars. The most luminous member is the ~2nd magnitude white-yellow supergiant Mirfak, also known as Alpha Persei. Bright members also include Delta, Sigma, Psi, 29, 30, 34, and 48 Persei.
The bolometric luminosity, summed over all wavelengths, is calculated from integrating the spectral energy distribution (SED) to be , making μ Cephei one of the most luminous red supergiants in the Milky Way. Its effective temperature of , determined from colour index relations, implies a radius of . Other recent publications give similar effective temperatures. Calculation of the luminosity from a visual and infrared colour relation give and a corresponding radius of .
The high orbital eccentricity of the pair allows astronomers to observe changes the colliding winds as their separation varies. Another prominent example of a colliding-wind binary is thought to be Eta Carinae, one of the most luminous objects in the Milky Way galaxy. The first colliding-wind binary to be detected in the X-ray band outside the Milky Way galaxy was HD 5980, located in the Small Magellanic Cloud.
The trailing 'c' describes the spiral arm structure as being loosely wound. The peculiar nature of the galaxy is noted with the 'pec.' abbreviation. The galaxy is bright at the center, with two nearly symmetrical inner spiral arms. It is a luminous infrared source, with total infrared luminosity is , ranking 55th in the 2003 IRAS Revised Bright Galaxy Sample, and is the second most luminous galaxy within 75 Mpc.
Wray 17-96 is a very luminous star in the Scorpius constellation, about away. It is a suspected luminous blue variable (LBV), although it has not shown the characteristic spectral variations. Wray 17-96 has an absolute bolometric magnitude of −10.9 (1.8 million solar units), making it one of the most luminous stars known. The spectral type is peculiar, showing emission and absorption, sometimes both in the same line.
HD 221776 is a double star in the northern constellation of Andromeda. With an apparent visual magnitude of 6.18,, it is viewable by the naked eye user very favourable conditions. The most luminous component has a spectral classification K5III, meaning that it's an orange giant star that has evolved off the main sequence. An infrared excess has been detected around this star, indicating the star is associated with a cloud of dust particles.
These are yellow supergiant stars (actually low mass post-AGB stars at the most luminous stage of their lives) which have alternating deep and shallow minima. This double-peaked variation typically has periods of 30–100 days and amplitudes of 3–4 magnitudes. Superimposed on this variation, there may be long-term variations over periods of several years. Their spectra are of type F or G at maximum light and type K or M at minimum brightness.
One is that ellipticals generally contain the most massive black holes, and so are capable of powering the most luminous active galaxies (see Eddington luminosity). Another is that ellipticals generally inhabit richer environments, providing a large-scale intergalactic medium to confine the radio source. It may also be that the larger amounts of cold gas in spiral galaxies in some way disrupts or stifles a forming jet. To date there is no compelling single explanation for the observations.
W49B is a supernova remnant (SNR) located roughly 33,000 light-years from Earth, Radio wavelengths show a shell four arc minutes across. There are infrared "rings" (about 25 light-years in diameter) forming a "barrel", and intense X-ray radiation coming from forbidden emission of nickel and iron in a bar along its axis. W49B is also one of the most luminous SNRs in the galaxy at gamma-ray wavelengths. It is invisible at optical wavelengths.
HV 888, also known as WOH S140, is a red supergiant (RSG) star located in the Large Magellanic Cloud. It is among the largest known stars, with a radius more than a thousand solar radii, and is also one of most luminous of its type with around 300,000 times the Sun's luminosity. The effective temperature is estimated to be around 3,500 K. If placed at the center of the solar system, its photosphere would engulf the orbit of Jupiter.
The emission lines are generated in the stellar wind and the photosphere is completely hidden. The surface fraction of hydrogen is still estimated to be around 60%. HD 97950B is the most massive and most luminous star known in the NGC 3603 region, nearly three million times more luminous than the sun and 132 times more massive. Although the star is very young, around 1.5 million years old, it has already lost a considerable fraction of its initial masses.
R99 (HD 269445) is a star in the Large Magellanic Cloud in the constellation Dorado. It is classified as a possible luminous blue variable and is one of the most luminous stars known. R99 has a peculiar spectrum that has been described as OBf:pe, "unclassifiable", peculiar WN10, "similar to the unusual LBV HD 5980", "unique", and Ofpe/WN9. The Ofpe/WN9 type remains even though other stars of this type have been reclassified to types between WN9 and WN11.
HD 143183 is a red supergiant variable star of spectral type M3Ia in constellation Norma. It is a member of the Norma OB1 association, at a distance of about 2 kiloparsecs. It is one of the most luminous red supergiants with a luminosity over 100,000 times greater than the Sun (), and is as well one of the largest stars with a radius more than a thousand times that of the Sun (). Older studies frequently calculated higher luminosities and radii.
The properties of V354 Cephei are disputed, but the star is classed as a cool supergiant star with a spectral and luminosity class given as M2.5 Iab, indicating it is an intermediate-size luminous supergiant, but was later given as M3.5 Ib, indicating it is rather a less luminous supergiant. A 2005 study led by Levesque described the four red supergiant stars, KW Sagittarii, V354 Cephei, KY Cygni and Mu Cephei as the largest and most luminous galactic red supergiants with radii of roughly and bolometric luminosity of roughly , which is consistent with the empirical upper radius and luminosity boundary for the red supergiants. Despite it, larger sizes and luminosities have been published for few other galactic red supergiants, such as VV Cephei A and the peculiar star VY Canis Majoris at and . V354 Cephei, based on a MARCS model, was found to be the largest and most luminous of these four stars measured, with a high luminosity of and consequently very large size of based on the assumption of an effective temperature of .
Aquila X-1 (frequently abbreviated to Aql X-1) is a low-mass x-ray binary (LMXB) and the most luminous X-Ray source in the constellation Aquila. It was first observed by the satellite Vela 5B which detected several outbursts from this source between 1969 and 1976. Its optical counterpart is variable, so it was named V1333 Aql according to the IAU standards. The system hosts a neutron star that accretes matter from a main sequence star of spectral type K4.
The spectrum of R71 in quiescence (minimum brightness) shows weak emission lines of Hα and Hβ and absorption lines for the rest of the Balmer series. There are many strong forbidden emission lines, especially of ionised iron. The spectrum is readily classified as a B class supergiant, the peculiarities such as emission and forbidden lines not unusual for the most luminous stars. During the 1970s outburst, many spectral lines developed strong P Cygni profiles, while the forbidden emission lines weakened and eventually disappeared.
Rho Cassiopeiae (; ρ Cas, ρ Cassiopeiae) is a yellow hypergiant star in the constellation Cassiopeia. It is about from Earth, yet can still be seen by the naked eye as it is over 300,000 times brighter than the Sun. On average it has an absolute magnitude of −9.5, making it visually one of the most luminous stars known. Its diameter measures between 400 and 500 times that of the Sun, approximately 627,000,000 kilometers, or about twice the size of the Earth's orbit.
From left to right: the Sun (small, faint dot on the far left representing – too small to be visible in this thumbnail), the Pistol Star, Rho Cassiopeiae, Betelgeuse, and VY Canis Majoris. The orbits of Jupiter ( 5.23 AU) and Neptune ( 30.01 AU) are included for comparison. Rho Cassiopeiae is one of the most luminous yellow stars known. It is close to the Eddington luminosity limit and normally loses mass at around /yr, hundreds of millions of times the rate of the solar wind.
The four brightest stars in NGC 4755 are blue supergiant stars, with a red supergiant star at the centre. (ESO VLT) Supergiant stars can be identified on the basis of their spectra, with distinctive lines sensitive to high luminosity and low surface gravity. In 1897, Antonia C. Maury had divided stars based on the widths of their spectral lines, with her class "c" identifying stars with the narrowest lines. Although it was not known at the time, these were the most luminous stars.
A very small number of Mira variables and other late AGB stars have supergiant luminosity classes, for example α Herculis. Classical Cepheid variables typically have supergiant luminosity classes, although only the most luminous and massive will actually go on to develop an iron core. The majority of them are intermediate mass stars fusing helium in their cores and will eventually transition to the asymptotic giant branch. δ Cephei itself is an example with a luminosity of and a mass of .
Vega is the brightest star in the northern constellation of Lyra. It has the Bayer designation α Lyrae, which is Latinised to Alpha Lyrae and abbreviated Alpha Lyr or α Lyr. This star is relatively close at only 25 light-years from the Sun, and, together with Arcturus and Sirius, one of the most luminous stars in the Sun's neighborhood. It is the fifth-brightest star in the night sky, and the second-brightest star in the northern celestial hemisphere, after Arcturus.
The stars of the Eta Carinae system are completely obscured by dust and opaque stellar winds, with much of the ultraviolet and visual radiation shifted to infrared. The total electromagnetic radiation across all wavelengths for both stars combined is several million solar luminosities (). The best estimate for the luminosity of the primary is making it one of the most luminous stars in the Milky Way. The luminosity of Eta Carinae B is particularly uncertain, probably and almost certainly no more than .
De Jager did work on stars and solar physics, in relation to which he was a founding editor of the journal Solar Physics.A closing editorial of "Solar Physics" at the Harvard website In 1980 he was principal investigator of the Hard X-ray Imaging Spectrometer (HXIS) on board the Solar Maximum Mission satellite. His work on solar flares was often done in collaboration with Zdeněk Švestka. From 1978 onward de Jager did noted work on the most luminous stars, known as hypergiants.
While there was some praise for the opera's orchestral introduction, described by the critic from Teatri, arti e letteratura as the most "luminous" piece in the score, the rest of the music was criticized for its lack of imagination and originality. However, it was Carlo Pepoli's libretto that came in for the worst criticism. La Moda wrote that "it seems impossible that Maestro Vaccai, who lacks neither intelligence nor experience, would consent to set a mess like this to music."La Moda (25 February 1836) p. 67.
As the first stars, dwarf galaxies and quasars gradually form, the intense radiation they emit reionizes much of the surrounding universe; splitting the neutral hydrogen atoms back into a plasma of free electrons and protons for the first time since recombination and decoupling. Reionization is evidenced from observations of quasars. Quasars are a form of active galaxy, and the most luminous objects observed in the universe. Electrons in neutral hydrogen have a specific patterns of absorbing photons, related to electron energy levels and called the Lyman series.
The intrinsic S-type stars are on the most luminous portion of the asymptotic giant branch, a stage of their lives lasting less than a million years. Many are long period variable stars. The extrinsic S stars are less luminous and longer-lived, often smaller-amplitude semiregular or irregular variables. S stars are relatively rare, with intrinsic S stars forming less than 10% of asymptotic giant branch stars of comparable luminosity, while extrinsic S stars form an even smaller proportion of all red giants.
Atkinson wrote about this theory again in the 1930s, predicting that the most luminous stars should have a short lifetime. He also proposed that the elements found in the Universe could be built up by fusion in stars, and that white dwarf stars did not need a nuclear source of energy in order to shine. After World War II, he worked on astronomical instrumentation and positional astronomy. Atkinson's mechanical skills led to a commission to design an astronomical clock for York Minster, the York Minster astronomical clock.
Red supergiants are massive stars that have left the main sequence and greatly expanded and cooled. Their high luminosity and low surface gravity means they are rapidly losing mass. The most luminous red supergiants can lose mass quickly enough that they become hotter and smaller. In the most massive stars, this can result in the star evolving permanently away from the red supergiant stage to become a blue supergiant, but in some cases the star will execute a blue loop and return to being a red supergiant.
It is also one of the most luminous quasars known, with an absolute magnitude of −26.7, meaning that if it were only as distant as Pollux (~10 parsecs) it would appear nearly as bright in the sky as the Sun. Since the sun's absolute magnitude is 4.83, it means that the quasar is over 4 trillion times more luminous than the Sun at visible wavelengths. The mass of its central black hole has been measured to be 886 ± 187 million solar masses through broad emission-line reverberation mapping.
The first water megamaser was found in 1979 in NGC 4945, a galaxy in the nearby Centaurus A/M83 Group. The first hydroxyl megamaser was found in 1982 in Arp 220, which is the nearest ultraluminous infrared galaxy to the Milky Way. All subsequent OH megamasers that have been discovered are also in luminous infrared galaxies, and there are a small number of OH kilomasers hosted in galaxies with lower infrared luminosities. Most luminous infrared galaxies have recently merged or interacted with another galaxy, and are undergoing a burst of star formation.
The mass of the star is likely to be around 26 solar masses, according to a 2011 study by Ducati, Penteado, and Turcati. However, due to the uncertain nature of the binary system hypothesis, the true mass could be much different than this. If the star actually has a mass of 51 solar masses (the median mass reported by Hohle, Neuhäuser, and Schutz in 2010), the star's bolometric luminosity would be over 1 million solar luminosities, making it among the most luminous stars known, although data to support this mass is tenuous at best.
Left to right: a red dwarf, the Sun, a B-type main sequence star, and R136a1 It was from 2010 to 2020 that the star was recognised as the most massive and luminous star known. Previous estimates had placed the luminosity as low as . At around , R136a1 is one of the most luminous stars known, radiating more energy in five seconds than the Sun does in a year. If it replaced the Sun in the Solar System, it would outshine the Sun by 164,000 times (MV = −8.2) and would appear from Earth at magnitude −40.
The Westerlund 1 magnetar is the most luminous X-ray point source in the cluster, with the sgB[e] star W9, the (presumed) binary W30a and the Wolf–Rayet stars WR A and WR B all strong X-ray sources. Approximately 50 other X-ray point sources are associated with luminous optical counterparts. Finally, at radio wavelengths the sgB[e] star W9 and red supergiants W20 and W26 are strong radio sources, while the majority of the cool hypergiants and a few OB supergiants and Wolf–Rayet stars are also detected.
The yellow hypergiant is an expected phase of evolution as the most luminous red supergiants evolve bluewards, but they may also represent a different sort of star. LBVs during eruption have such dense winds that they form a pseudo-photosphere which appears as a larger cooler star despite the underlying blue supergiant being largely unchanged. These are observed to have a very narrow range of temperatures around 8,000K. At the bistability jump which occurs around 21,000K blue supergiant winds become several times denser and could be result in an even cooler pseudo-photosphere.
Hubble to find a distant supernova. The "SN 2003fg" was discovered in a forming galaxy in 2003. The appearance of this supernova was studied in "real-time", and it has posed several major physical questions as it seems more massive than the Chandrasekhar limit would allow. First observed in September 2006, the supernova SN 2006gy, which occurred in a galaxy called NGC 1260 (240 million light-years away), is the largest and, until confirmation of luminosity of SN 2005ap in October 2007, the most luminous supernova ever observed.
In 1865–1866, Dana conducted the newly established and unsuccessful Chicago Republican, when the paper was owned by Jacob Bunn, and published by Alonzo Mack. He became the editor and part-owner of The Sun (New York) in 1868, and remained in control of it until his death.Mott, 1960, pp. 373-374 Upon taking control over the organization, he announced his credo: > It will study condensation, clearness, point, and will endeavor to present > its daily photograph of the whole world's doings in the most luminous and > lively manner.
ASASSN-15lh (supernova designation SN 2015L) is an extremely luminous astronomical transient discovered by the All Sky Automated Survey for SuperNovae (ASAS-SN), with the appearance of a superluminous supernova event. It was first detected on June 14, 2015, located within a faint galaxy in the southern constellation Indus, and was the most luminous supernova-like object ever observed. At its peak, ASASSN-15lh was 570 billion times brighter than the Sun, and 20 times brighter than the combined light emitted by the Milky Way Galaxy. The emitted energy was exceeded by PS1-10adi.
APM 08279+5255 was initially identified as a quasar in 1998 during an Automatic Plate Measuring Facility (APM) survey to find carbon stars in the galactic halo. The combination of its high redshift (z=3.87) and brightness (particularly in the infrared) made it the most luminous object yet seen in the universe. It was suspected of being a gravitationally lensed object, with its luminosity magnified. Observations in the infrared with the NICMOS high- resolution camera on board the Hubble Space Telescope (HST) showed that the source was composed of three discrete images.
Cygnus OB2 #12 is an extremely bright blue hypergiant with an absolute bolometric magnitude (all electromagnetic radiation) of −10.9, among the most luminous stars known in the galaxy. This makes the star nearly two million times more luminous than the Sun, although less than half the estimates when the star was first discovered. It is now known to be a binary, with the companion approximately a tenth as bright. A very approximate initial estimate of the orbit gives the total system mass as and the period as 30 years.
NGC 3603-B (HD 97950B) is a Wolf-Rayet star located at the centre of the HD 97950 cluster in the NGC 3603 star-forming region, about 25,000 light years from Earth. It has the spectral type WN6h and is among the most luminous and most massive stars known. HD 97950 was catalogued as a star, but was known to be a dense cluster or close multiple star. In 1926, the six brightest members were given letters from A to F, although several of them have since been resolved into more than one star.
The location of the companion resolved in the near-infrared is slightly further from the primary than the radio source originally called WR 147N, and it has been referred to as WR 147NIR. The Wolf-Rayet star in the system (WR 147S) has a luminosity of , making it one of the most luminous stars known. The B-type companion is much less luminous, at . The orbital elements of WR 147's orbit are poorly known, as the two components are separated far enough that no orbital motion has been detected.
These are not massive stars, though; instead, they are stars of intermediate mass that have particularly low surface gravities, often due to instability such as Cepheid pulsations. These intermediate mass stars' being classified as supergiants during a relatively long-lasting phase of their evolution account for the large number of low luminosity yellow supergiants. The most luminous yellow stars, the yellow hypergiants, are amongst the visually brightest stars, with absolute magnitudes around −9, although still less than . There is a strong upper limit to the luminosity of red supergiants at around .
NGC 3603-A1 (HD 97950A1) is a double-eclipsing binary star system located at the centre of the HD 97950 cluster in the NGC 3603 star-forming region, about 25,000 light years from Earth. Both stars are of spectral type WN6h and among the most luminous and most massive known. HD 97950 was catalogued as a star, but was known to be a dense cluster or close multiple star. In 1926, the six brightest members were given letters from A to F, although several of them have since been resolved into more than one star.
The light curve produced by the eruption is unlike anything previously seen. In 2009 the star was about , which in the absence of extinction would correspond to an apparent magnitude of 8.5 Comparison between the size of V838 Monocerotis and the Inner Solar System. The star brightened to about a million times solar luminosity and absolute magnitude of −9.8, ensuring that at the time of maximum V838 Monocerotis was one of the most luminous stars in the Milky Way galaxy. The brightening was caused by a rapid expansion of the outer layers of the star.
These parameters make Westerlund 1-26 one of most luminous red supergiants and are also similar to those estimated for another notable red supergiant star, VY Canis Majoris. An earlier calculation of the luminosity and the temperature by fitting the spectral energy distribution and based on the spectrum by using DUSTY model gave a far much higher luminosity of just around and a photospheric temperature of , which all correspond to a very large radius of and is considerably more luminous than expected for any red supergiant and extreme.
HD 5980 is a multiple star system on the outskirts of NGC 346 in the Small Magellanic Cloud (SMC) and is one of the brightest stars in the SMC. HD 5980 has at least three components among the most luminous stars known: the unusual primary has a Wolf–Rayet spectrum and has produced a luminous blue variable (LBV) outburst; the secondary, also a Wolf–Rayet star, forms an eclipsing spectroscopic binary with the primary star; and a more distant O-type supergiant is also likely to be a binary.
Hypernovae are now widely accepted to be supernovae with ejecta having a kinetic energy larger than about , an order of magnitude higher than a typical core collapse supernova. The ejected nickel masses are large and the ejection velocity up to 99% of the speed of light. These are typically of type Ic, and some are associated with long-duration gamma-ray bursts. The electromagnetic energy released by these events varies from comparable to other type Ic supernova, to some of the most luminous supernovae known such as SN 1999as.
Optical and ultraviolet images of the black hole in the center of NGC 4151, a Seyfert Galaxy An active galactic nucleus (AGN) is a compact region at the center of a galaxy that has a higher than normal luminosity over portions of the electromagnetic spectrum. A galaxy having an active nucleus is called an active galaxy. Active galactic nuclei are the most luminous sources of electromagnetic radiation in the Universe, and their evolution puts constraints on cosmological models. Depending on the type, their luminosity varies over a timescale from a few hours to a few years.
In the (sub)tropics it can be seen at its clearest from September to early November, and at low southern, tropical, latitudes of less than 25°S it can be seen, seasonally, low in the North. At magnitude 2.2, Alpha Cassiopeiae, or Schedar, is generally the brightest star in Cassiopeia, though it is occasionally outshone by the variable Gamma Cassiopeiae, which has reached magnitude 1.6. The constellation hosts some of the most luminous stars known, including the yellow hypergiants Rho Cassiopeiae and V509 Cassiopeiae and white hypergiant 6 Cassiopeiae. In 1572, Tycho Brahe's supernova flared brightly in Cassiopeia.
The last stars in the list are familiar nearby stars put there for comparison, and not among the most luminous known. It may also interest the reader to know that the Sun is more luminous than approximately 95% of all known stars in the local neighbourhood (out to, say, a few hundred light years), due to enormous numbers of somewhat less massive stars that are cooler and often much less luminous. For perspective, the overall range of stellar luminosities runs from dwarfs less than 1/10,000th as luminous as the Sun to supergiants over 1,000,000 times more luminous.
The IUE Mega Campaign: Wind Structure and Variability of HD 50896 (WN5) Astrophysical Journal Letters 452 #1, pp. L57 (October 1995) VY Canis Majoris is a remote red hypergiant located approximately 3,800 light-years away from Earth. It is one of largest stars known (sometimes described as the largest known) and is also one of most luminous with a radius varying from 1,420 to 2,200 times the Sun's radius, and a luminosity around 300,000 times greater than the Sun. Its current mass is about 17 ± 8 solar masses, having shed material from an initial mass of 25–32 solar masses.
MY Cephei (IRC +60375) is a red supergiant located in open cluster NGC 7419 in the constellation of Cepheus. It is a semiregular variable star with a maximum brightness of magnitude 14.4 and a minimum of magnitude 15.5. MY Cephei has an unusual spectral type of M7.5, one of the latest spectral types of any supergiant, and is one of the most luminous and coolest red supergiants, as well as one of the largest known stars. If placed at the center of the Solar System, the star's surface would engulf the orbit of Jupiter and possibly even the orbit of Saturn.
The most luminous stars are always young stars, no more than a few million years for the most extreme. In the Hertzsprung–Russell diagram, the x-axis represents temperature or spectral type while the y-axis represents luminosity or magnitude. The vast majority of stars are found along the main sequence with blue Class O stars found at the top left of the chart while red Class M stars fall to the bottom right. Certain stars like Deneb and Betelgeuse are found above and to the right of the main sequence, more luminous or cooler than their equivalents on the main sequence.
High-speed photography showing different parts of a lightning flash during the discharge process as seen in Toulouse, France. Once a conductive channel bridges the air gap between the negative charge excess in the cloud and the positive surface charge excess below, there is a large drop in resistance across the lightning channel. Electrons accelerate rapidly as a result in a zone beginning at the point of attachment, which expands across the entire leader network at up to one third of the speed of light. This is the 'return stroke' and it is the most luminous and noticeable part of the lightning discharge.
3C 454.3 is a blazar (a type of quasar with a jet oriented toward Earth) located away from the galactic plane. It is one of the brightest gamma ray sources in the sky, and is the most luminous astronomical object ever observed, with a maximum absolute magnitude of -31.4. It has the brightest blazar gamma ray flare recorded, twice as bright as the Vela Pulsar in the Milky Way galaxy. It also flares at radio and visible wavelengths – in red light, the blazar brightened by more than 2.5 times to magnitude 13.7 – and it is very bright at high radio frequencies.
The Mango Tree enjoyed reasonable success, grossing $1,028,000 at the box office in Australia,Film Victoria - Australian Films at the Australian Box Office which is equivalent to $4,728,800 in 2009 dollars. Critical reaction was muted, with much criticism falling on the performance of Christopher Pate. However film writer Brian McFarlane later wrote that Geraldine Fitzgerald gave "one of the most luminous performances by an actress in Australian film."Brian McFarlane, 'The choice fruit of The Mango Tree (Kevin James Dobson, 1977)', Senses of Cinema, 11 July 2010 accessed 28 September 2012 The movie achieved only limited sales overseas.
The Extremely Luminous Infrared Galaxy WISE J224607.57-052635.0, with a luminosity of 300 trillion suns was discovered by NASA's Wide-field Infrared Survey Explorer (WISE), and as of May 2015 is the most luminous galaxy found. The galaxy belongs to a new class of objects discovered by WISE, extremely luminous infrared galaxies, or ELIRGs. Light from the WISE J224607.57-052635.0 galaxy has traveled 12.5 billion years. The black hole at its center was billions of times the mass of our sun when the universe was a tenth (1.3 billion years) of its present age of 13.8 billion years.
The Great Observatories All-sky LIRG Survey (GOALS) is a multi-wavelength study of luminous infrared galaxies, incorporating observations with NASA's Great Observatories and other ground and space-based telescopes. Using information from NASA's Spitzer, Hubble, Chandra and Galex observations in a study over 200 of the most luminous infrared selected galaxies in the local universe. Approximately 180 LIRGs were identified along with over 20 ULIRGs. The LIRGs and ULIRGs targeted in GOALS span the full range of nuclear spectral types (type-1 and type 2 Active Galactic Nuclei, LINERS's, and starbursts) and interaction stages (major mergers, minor mergers, and isolated galaxies).
HXMM01, known more formally as 1HERMES S250 J022016.5−060143, is a starburst galaxy located in the northwestern portion of the constellation Cetus.Inferred from right ascension and declination of galaxy using the Fourmilab Virtual Telescope. Discovered in 2013 by a team at the University of California, Irvine, it was discovered that HXMM01 is actually still forming from its two parent galaxies as part of the "brightest, most luminous and most gas-rich submillimeter-bright galaxy merger known." When the merger is complete, HXMM01 will rapidly evolve to become a giant elliptical galaxy with a mass about four times that of the Milky Way.
The Sotheby's Wine Encyclopedia (4th Edition) pg 180 Dorling Kindersley 2005 Henriot's cellar master Laurent Fresnet, who was named "Sparkling Winemaker of the Year" by International Wine Challenge in 2015 and 2016, has said: "What makes our champagne so special is that it is sourced from beautiful terroirs, mostly Grand & Premier Cru vineyards. Thanks to our independent status, I can dedicate the time and care they require to craft the most luminous champagnes and perpetuate the unique style of the House." The Henriot family also owns the producers Bouchard Père & Fils, William Fèvre and Château de Poncié in Burgundy and Chablis.
The most massive O-type stars develop a WNLh spectral type as they start to convect material from the core towards the surface, and these are the most luminous stars that exist. Low to intermediate-mass stars age in a very different way, through red-giant, horizontal-branch, asymptotic-giant-branch (AGB), and then post-AGB phases. Post-AGB evolution generally involves dramatic mass loss, sometimes leaving a planetary nebula, and leaving an increasingly hot exposed stellar interior. If there is sufficient helium and hydrogen remaining, these small but extremely hot stars have an O-type spectrum.
KW Sagittarii is classed as a luminous cool supergiant and varies its spectral type between M0 and M4. A 2005 study led by Levesque, using a MARCS model, calculated a high luminosity of for KW Sgr and consequently very large radius of based on the assumption of an effective temperature of . The star was then described as among the four largest and most luminous galactic red supergiants, which includes V354 Cephei, KY Cygni and Mu Cephei. More recently, KW Sagittarii was calculated to have a lower bolometric luminosity around and a radius around was based on the measured angular diameter and luminosity.
LBV 1806-20 is a candidate luminous blue variable (LBV) and likely binary star located around from the Sun, towards the center of the Milky Way. It has an estimated mass of around 36 solar masses and an estimated variable luminosity of around two million times that of the Sun. It is highly luminous but is invisible from the Solar System at visual wavelengths because less than one billionth of its visible light reaches us. When first discovered, LBV 1806-20 was considered both the most luminous and most massive star known, challenging our understanding of the formation of massive stars.
The two objects are the most luminous in their respective categories. For these reasons, and because of the important role it has repeatedly played in the modern era, SN 1054 is one of the best known supernovae in the history of astronomy. The Crab Nebula is easily observed by amateur astronomers thanks to its brightness, and was also catalogued early on by professional astronomers, long before its true nature was understood and identified. When the French astronomer Charles Messier watched for the return of Halley's Comet in 1758, he confused the nebula for the comet, as he was unaware of the former's existence.
R136c is a Wolf–Rayet star of the spectral type WN5h and with a temperature of 51,000 K, making it one of the hottest stars known. It is the most massive star known, with a mass of , and it is one of most luminous stars known, with a luminosity of 5.6 million . The extreme luminosity is produced by the CNO fusion process in its highly compressed hot core. Typical of all Wolf–Rayet stars, R136c has been losing mass by means of a strong stellar wind with speeds over 2,000 km/s and mass loss rates in excess of solar masses per year.
NGC 3603-C (HD 97950C) is a single-lined spectroscopic binary star system located at the centre of the HD 97950 cluster in the NGC 3603 star-forming region, about 25,000 light years from Earth. The primary has spectral type WN6h and is among the most luminous and most massive known. HD 97950 was catalogued as a star, but was known to be a dense cluster or close multiple star. In 1926, the six brightest members were given letters from A to F, although several of them have since been resolved into more than one star.
Supergiants are also evolved stars with higher levels of heavy elements than main-sequence stars. This is the basis of the MK luminosity system which assigns stars to luminosity classes purely from observing their spectra. In addition to the line changes due to low surface gravity and fusion products, the most luminous stars have high mass-loss rates and resulting clouds of expelled circumstellar materials which can produce emission lines, P Cygni profiles, or forbidden lines. The MK system assigns stars to luminosity classes: Ib for supergiants; Ia for luminous supergiants; and 0 (zero) or Ia+ for hypergiants.
Absolute magnitudes range from about −4, 3,400 times brighter than the sun, to about −5.8, 18,000 times brighter than the sun. Class O stars are very young, no more than a few million years old, and in our galaxy they all have high metallicities, around twice that of the sun. O-type main sequence stars in the Large Magellanic Cloud, with lower metallicity, have noticeably higher temperatures, with the most obvious cause being lower mass loss rates. The most luminous class O stars have mass loss rates of more than each year, although the least luminous lose far less.
NGC 1142 is one of most luminous galaxies in the local universe as far as CO emission is concerned, twice as bright as the merger remnant Arp 220. Most of the emission originates from the ring, and especially its southern part, and a giant HII region west of the nucleus. The nucleus of NGC 1142 has been found to be active and it has been categorised as a type II Seyfert galaxy. The most accepted theory for the energy source of active galactic nuclei is the presence of an accretion disk around a supermassive black hole.
This was completely unexpected for protostars, instead suggesting the objects were much more evolved stars. Shortly afterwards two emission line stars were classified as Wolf Rayet stars, and a third as a Luminous Blue Variable that was thought to be one of the most luminous stars in the galaxy. A small number of red supergiants were also identified, narrowing the likely age of the cluster. In 1999, a study of nearly 600 stars in the cluster showed that the Quintuplet contained more Wolf–Rayet stars than any known cluster, as well as a second Luminous Blue Variable.
Lewis undertakes a broad spectrum of research in astronomy and cosmology. On the largest scales, his program involves looking at the influence of dark energy and dark matter on the evolution and ultimate fate of the universe. Another aspect of Lewis's research uses the phenomenon of gravitational lensing to probe the nature and distribution of the pervasive dark matter, and employing individual stars to magnify the hearts of quasars, the most luminous objects in the universe. Closer to home, Lewis's research focuses upon galactic cannibalism, where small dwarf galaxies are torn apart by the much more massive Milky Way and Andromeda Galaxy.
George also designed many of the tail section costumes, including Nam's, using Japanese Boro fabric. In creating Claude's yellow coat and dress, George was mindful of the fact it was the first colour of brightness in the tail section scene, as well as the property of yellow being the most luminous colour in the spectrum. She expressed, "It's the colour that captures our attention more than any other and in colour psychology yellow is non-emotional and lacking compassion." Camera testing occurred before deciding the final colours as well as observing how they'd interact, with the back drop of darker costume colours.
In fact, it is difficult to explain even the small number of observed yellow hypergiants, relative to red supergiants of comparable luminosity, from simple models of stellar evolution. The most luminous red supergiants may execute multiple "blue loops", shedding much of their atmosphere, but without actually ever reaching the blue supergiant stage, each one taking only a few decades at most. Conversely, some apparent yellow hypergiants may be hotter stars, such as the "missing" LBVs, masked within a cool pseudo-photosphere. Recent discoveries of blue supergiant supernova progenitors have also raised the question of whether stars could explode directly from the yellow hypergiant stage.
Increased luminosity at the same temperature, or alternatively cooler temperature at the same luminosity, indicates that these stars are larger than those on the main sequence and they are called giants or supergiants. Blue and white supergiants are high luminosity stars somewhat cooler than the most luminous main sequence stars. A star like Deneb, for example, has a luminosity around 200,000 L⊙, a spectral type of A2, and an effective temperature around 8,500 K, meaning it has a radius around . For comparison, the red supergiant Betelgeuse has a luminosity around 100,000 L⊙, a spectral type of M2, and a temperature around 3,500 K, meaning its radius is about .
SMC 018136, also known as PMMR 37, is a red supergiant star located in the Small Magellanic Cloud. It is one of the largest stars and one of most luminous SMC cool supergiants so far discovered, with a radius of 1,310 times that of the sun and a bolometric luminosity over 200,000 times more than Sun. If it were in the place of the Sun, its photosphere would at least engulf the orbit of Jupiter. SMC 018136 has a spectral type M0 Ia and an effective temperature 3,575 K, although more recent papers suggest it has a slightly earlier spectral type of K4.5 Ia-Ib.
This is towards the upper end of values published over the past few decades, which vary between and . Deneb is the most luminous first magnitude star, that is, stars with a brighter apparent magnitude than 1.5. Deneb is also the most distant of the 30 brightest stars by a factor of almost 2. Based on its temperature and luminosity, and also on direct measurements of its tiny angular diameter (a mere 0.002 seconds of arc), Deneb appears to have a diameter of about over 200 times that of the Sun; if placed at the center of the Solar System, Deneb would extend out to the orbit of the Earth.
Supernova impostors appear as remarkably faint supernovae of spectral type IIn—which have hydrogen in their spectrum and narrow spectral lines that indicate relatively low gas speeds. These impostors exceed their pre-outburst states by several magnitudes, with typical peak absolute visual magnitudes of −11 to −14, making these outbursts as bright as the most luminous stars. The trigger mechanism of these outbursts remains unexplained, though it is thought to be caused by violating the classical Eddington luminosity limit, initiating severe mass loss. If the ratio of radiated energy to kinetic energy is near unity, as in Eta Carinae, then we might expect an ejected mass of about 0.16 solar masses.
A hot, dust-obscured galaxy seen by WISE Luminosity plot for hot DOGs and a prototypical luminous infrared galaxy A hot, dust-obscured galaxy, or hot DOG, is a rare type of quasar. The central black hole of such a galaxy emits vast amounts of radiation which heats the infalling dust and gas, releasing infrared light at a rate about 1,000 times as much as the Milky Way, making these some of the most luminous galaxies in the universe. However, the density of the surrounding dust is so great that most of that light is obscured. Their average temperatures range from , significantly higher than an average galaxy's temperature of .
Photographic plates of blue light from the galaxy (sampling stars excluding the diffuse halo) yield an effective radius (the radius within which half the light is emitted) of . The galaxy has a very large halo of much lower intensity "diffuse light" extending to a radius of . The authors of the study identifying the halo conclude that IC 1101 is "possibly one of the largest and most luminous galaxies in the universe". Like most large galaxies, IC 1101 is populated by a number of metal-rich stars, some of which are seven billion years older than the Sun, making it appear golden yellow in color.
HV 11423 is one of largest known stars with an estimated radius over 1,000 times larger than the sun. It is also a variable star with a variation of up 2 magnitudes at visual wavelengths but essentially constant in the infrared. It is listed in the General Catalogue of Variable Stars as a slow irregular variable, but a period of 720 days has been calculated, as well as a long secondary period of 1,817 days. The bolometric luminosity is over 300,000 times more than Sun, making it one of most luminous cool supergiants, and appears to have remained unchanged during the brightness and spectral variations.
NGC 2363-V1 is a luminous blue variable star in the star-forming region NGC 2363, at the far southwestern part of the irregular galaxy NGC 2366 in the constellation Camelopardalis, near the North Celestial Pole approaching 11 million light years away from our galaxy. It was discovered in 1996 by Laurent Drissen, Jean-René Roy, and Carmelle Robert while examining images taken by the Hubble Space Telescope Wide Field Planetary Camera 2. NGC 2363-V1 is one of the most luminous stars known. It has been undergoing an increase in temperature and luminosity for the last 20 years, after a dramatic increase in its rate of mass loss.
One of the galaxy clusters, MACS J0647+7015 was found to have gravitationally lensed the most distant galaxy (MACS0647-JD) then ever imaged, in 2012, by CLASH. The first statistical study of X-ray cavities in distant clusters of galaxies was performed by analyzing the Chandra X-ray observations of MACS. Out of 76 clusters representing a sample of the most luminous X-ray clusters, observers found 13 cut and clear cavities and 7 possible cavities. A new radio halo, as well as a relic applicant, were found in MACS, with the help of the Giant Meterwave Radio Telescope and the Karoo Array Telescope-7.
Supergiants are rare and short-lived stars, but their high luminosity means that there are many naked- eye examples, including some of the brightest stars in the sky. Rigel, the brightest star in the constellation Orion is a typical blue-white supergiant; Deneb is the brightest star in Cygnus, a white supergiant; Delta Cephei is the famous prototype Cepheid variable, a yellow supergiant; and Betelgeuse, Antares and UY Scuti are red supergiants. μ Cephei is one of the reddest stars visible to the naked eye and one of the largest in the galaxy. Rho Cassiopeiae, a variable, yellow hypergiant, is one of the most luminous naked- eye stars.
SDSS J0100+2802 is about four times more luminous than SDSS J1148+5251, and seven times more luminous than ULAS J1120+0641, the most distant quasar known, although it is only less than fourth as luminous as HS 1946+7658, the most luminous quasar known. It harbors a black hole with mass of 12 billion solar masses (estimated according to MgII emission line correlations). This makes it one of the most massive black holes discovered so early in the universe, although it is only less than one fifth as massive as TON 618, the most massive black hole known. The diameter of this black hole is about 70.9 billion kilometres, seven times the diameter of Pluto's orbit.
Usually, this results in the total system luminosity being reduced and spread among several components. These binaries are common both because the conditions that produce high mass high luminosity stars also favour multiple star systems, but also because searches for highly luminous stars are inevitably biased towards detecting systems with multiple more normal stars combining to appear luminous. Because of all these problems, other references may give very different lists of the most luminous stars (different ordering or different stars altogether). Data on different stars can be of somewhat different reliability, depending on the attention one particular star has received as well as largely differing physical difficulties in analysis (see the Pistol Star for an example).
H-band infrared image of 1806-20 cluster 1806-20 (originally named the SGR 1806-20 cluster) is a heavily obscured star cluster on the far side of the Milky Way, approximately 50,000 light years distant. It contains the Soft gamma repeater SGR 1806-20 and the luminous blue variable hypergiant LBV 1806-20, a candidate for the most luminous star in the Milky Way. LBV 1806-20 and many of the other massive stars in the cluster are thought likely to end as supernovas in a few million years, leaving only neutron stars or black holes as remnants. The cluster is heavily obscured by intervening dust, and mostly visible in the infrared.
The FK Com stars are giants of spectral type K with an unusually rapid rotation and signs of extreme activity. Their X-ray coronae are among the most luminous (LX ≥ 1032 erg·s−1 or 1025 W) and the hottest known with dominant temperatures up to 40 MK. However, the current popular hypothesis involves a merger of a close binary system in which the orbital angular momentum of the companion is transferred to the primary. Pollux is the brightest star in the constellation Gemini, despite its Beta designation, and the 17th brightest in the sky. Pollux is a giant orange K star that makes an interesting color contrast with its white "twin", Castor.
Belinda J. Wilkes is a Senior Astrophysicist at the Smithsonian Astrophysical Observatory (SAO) in Cambridge, Massachusetts, US, and current director of the Chandra X-ray Center. She was born in Staffordshire, England and grew up in Albrighton, Shropshire, attending Wolverhampton Girls' High School before studying Physics and Astronomy at the University of St. Andrews, Scotland followed by a PhD in Astronomy from the University of Cambridge, England. In 1982 she moved to the University of Arizona's Steward Observatory as a NATO postdoctoral fellow and in 1984 to SAO's High Energy Astrophysics Division. Her research relates to multi-wavelength studies of quasars: galaxies containing super-massive black holes at their centers and the most luminous sources in the Universe.
While this is partly due to interstellar absorption, any tight clustering of stars at such a great distance in the galactic plane would be scarcely distinguishable from the general background. A study published in 2014, where the VLT has been used among other instruments, shows the presence of a very massive star in the central cluster of this star-forming region. The parameters of said star (W49nr1) are so far poorly constrained, but a luminosity of several million times that of the Sun is estimated as well as an initial mass between 100 and 180 solar masses, and perhaps even more, what would place it among both the most luminous and massive stars known.
This allows the telescopes to rapidly repoint towards a GRB, often within seconds of receiving the signal and while the gamma-ray emission itself is still ongoing.Akerlof 2003Akerlof 1999 New developments since the 2000s include the recognition of short gamma-ray bursts as a separate class (likely from merging neutron stars and not associated with supernovae), the discovery of extended, erratic flaring activity at X-ray wavelengths lasting for many minutes after most GRBs, and the discovery of the most luminous (GRB 080319B) and the former most distant (GRB 090423) objects in the universe.Bloom 2009Reddy 2009 The most distant known GRB, GRB 090429B, is now the most distant known object in the universe.
In Self-Portrait with Beret and Turned-Up Collar Rembrandt is seated in a broadly painted fur cloak, his hands clasped in his lap. Light from the upper right fully illuminates the face, hollowing the form of the cheek, and allowing for the representation of blemishes on the right cheek and ear lobe.White, 200 The picture is painted in a restrained range of browns and grays, enriched by a red shape that probably indicates the back of his chair, while another red area at the lower left corner of the canvas may be a tablecloth.White, 200 The most luminous area, the artist's face, is framed by a large beret and the high collar that flatteringly hides his jowls.
These are giants of spectral types G and K with an unusually rapid rotation and signs of extreme activity. Their X-ray coronae are among the most luminous (Lx ≥ 1032 erg·s−1 or 1025W) and the hottest known with dominant temperatures up to 40 MK. The astronomical observations planned with the Einstein Observatory by Giuseppe Vaiana and his group showed that F-, G-, K- and M-stars have chromospheres and often coronae much like our Sun. The O-B stars, which do not have surface convection zones, have a strong X-ray emission. However these stars do not have coronae, but the outer stellar envelopes emit this radiation during shocks due to thermal instabilities in rapidly moving gas blobs.
Its most luminous members are and , with both having luminosities several million times that of the Sun, and there are three other extreme stars with O3 spectral classes. Both and are binaries, with the primary stars contributing most of the luminosity, but with companions which are themselves more massive and luminous than most stars. Totalling all wavelengths, is estimated to be the more luminous of the two, 6,300,000 times the Sun's luminosity (absolute bolometric magnitude -12.25) compared to at 5,000,000 times the Sun's luminosity (absolute bolometric magnitude -12.0). However, appears by far the brightest object, both because it is brighter in visual wavelengths and because it is embedded in nebulosity which exaggerates the luminosity.
Stephenson 2-18 (St2-18), also known as Stephenson 2 DFK 1 or RSGC2-18, is a red supergiant star in the constellation of Scutum. It lies near the open cluster Stephenson 2, which is located around 6,000 parsecs (20,000 ly) away from Earth, and is assumed to be one of a group of stars at a similar distance. It is among the largest known stars, if not the largest, and one of the most luminous red supergiants, with an estimated radius around 2,150 times that of the Sun (), which corresponds to a volume around 10 billion times bigger than the Sun. If placed at the center of the Solar System, its photosphere would engulf the orbit of Saturn.
Although quasars appear faint when viewed from Earth, they are visible from extreme distances, being the most luminous objects in the known universe. The brightest quasar in the sky is 3C 273 in the constellation of Virgo. It has an average apparent magnitude of 12.8 (bright enough to be seen through a medium-size amateur telescope), but it has an absolute magnitude of −26.7. From a distance of about 33 light- years, this object would shine in the sky about as brightly as our Sun. This quasar's luminosity is, therefore, about 4 trillion (4) times that of the Sun, or about 100 times that of the total light of giant galaxies like the Milky Way.
The nucleus of this galaxy is an H II region, and it contains an ultraluminous X-ray source with an emission of , which is the most luminous source of X-rays in the Local Group of galaxies. This source is modulated by 20% over a 106-day cycle. However, the nucleus does not appear to contain a supermassive black hole, as an upper limit of 3,000 solar masses is placed on the mass of a central black hole based upon the velocity of stars in the core region. The inner part of the galaxy has two luminous spiral arms, along with multiple spurs that connect the inner to the outer spiral features.
The Times Literary Supplement, in a review of Davies' poem "The Ophthalmologist", writes "we might read this whole piece as an extended metaphor for the agony and ecstasy intrinsic to every creative act." A Contemporary Poetry Review review of New British Poetry discussing poet omissions from the collection writes "I, for one, particularly regret the neglect of the underrated Hilary Davies, whose first book, The Shanghai Owner of the Bonsai Shop ... contains some of the most luminous and quietly compelling poems you’ll come across on either side of the Atlantic." In a Valley of This Restless Mind has been called "a collection of high seriousness" and compared to the poetry of Elizabeth Jennings.
WOH G64 (IRAS 04553-6825) is a red supergiant (RSG) star in the Large Magellanic Cloud (LMC) satellite galaxy in the southern constellation of Dorado. It is one of the largest known stars and one of the most luminous and massive red supergiants, with a radius over 1,500 times that of the Sun () and a luminosity varying from 300,000 to 600,000 times the solar luminosity (). WOH G64 is surrounded by an optically thick dust envelope of roughly a light year in diameter containing 3 to 9 times the Sun's mass of expelled material that was created by the strong stellar wind. If placed at the center of the Solar System, the star's surface would engulf the orbit of Jupiter.
However, recent work by researchers at the Max Planck Institute for Astrophysics suggests that the GRXE may indeed consist of an additional, diffuse component after all. This diffuse component could arise not from the thermal emission of a very hot plasma but from the reprocessing by the interstellar gas of the X-ray radiation produced by luminous X-ray binary sources located in the Galaxy. X-ray binaries are the most luminous sources of X-rays in galaxies such as the Milky Way. These binary systems emit X-ray radiation when material or substance from a so-called donor star falls into the strong gravitational field of a compact object, such as a neutron star or a black hole.
BP Crucis is around 43 times as massive as the Sun, it is also one of the most luminous stars known in the Galaxy, with an estimated bolometric luminosity of around 470,000 times that of the Sun and a radius 70 times that of the Sun. The neutron star appears to belong to the "high mass" variety being at least . It is very likely to have a mass less than as the theoretical maximum mass based on the equation of state for a neutron star. The pulsar has a spin period of 685 seconds, but shows relatively large spindown rates thought to be due to its strong magnetic field, and also occasional spinups due to interaction with the accretion disk.
For a long time, active galaxies held all the records for the highest-redshift objects known either in the optical or the radio spectrum, because of their high luminosity. They still have a role to play in studies of the early universe, but it is now recognised that an AGN gives a highly biased picture of the "typical" high- redshift galaxy. Most luminous classes of AGN (radio-loud and radio-quiet) seem to have been much more numerous in the early universe. This suggests that massive black holes formed early on and that the conditions for the formation of luminous AGN were more common in the early universe, such as a much higher availability of cold gas near the centre of galaxies than at present.
For the most luminous of distance indicators, the Type Ia supernovae, this homogeneity is known to be poor; however, no other class of object is bright enough to be detected at such large distances, so the class is useful simply because there is no real alternative. The observational result of Hubble's Law, the proportional relationship between distance and the speed with which a galaxy is moving away from us (usually referred to as redshift) is a product of the cosmic distance ladder. Edwin Hubble observed that fainter galaxies are more redshifted. Finding the value of the Hubble constant was the result of decades of work by many astronomers, both in amassing the measurements of galaxy redshifts and in calibrating the steps of the distance ladder.
Daily Telegraph (1 July 1993) Dan Jacobson wrote that Wheldon "had a gift for friendship";Obituary, Jacqueline Wheldon, The Times (24 June 1993) Melvyn Bragg used precisely the same words, adding that "she was one of the very few clever people who was also good".Obituary, Independent (28 June 1993) Norman Podhoretz wrote: "I have known a few people of genius... but of them all, she was the most luminous." "I’m very interested in what God is," she once said, "interested in the idea that God is profound experience".M. Pugh, Enter the Girl with a Nose for Disaster, Daily Mail (9 February 1966) By 1976 she had faith enough to write a prayer for her husband during a dire illness.
Many R Coronae Borealis variables, although not all, are yellow supergiants, but this variability is due to their unusual chemical composition rather than a physical instability. Further types of variable stars such as RV Tauri variables and PV Telescopii variables are often described as supergiants. RV Tau stars are frequently assigned spectral types with a supergiant luminosity class on account of their low surface gravity, and they are amongst the most luminous of the AGB and post-AGB stars, having masses similar to the sun; likewise, the even rarer PV Tel variables are often classified as supergiants, but have lower luminosities than supergiants and peculiar B[e] spectra extremely deficient in hydrogen. Possibly they are also post-AGB objects or "born-again" AGB stars.
This is a massive supergiant star with a stellar classification of B3 Ia, indicating that, at the age of around 7 million years, it has exhausted the supply of hydrogen at its core and is now undergoing nuclear fusion of helium to generate energy. It has about 21 times the mass of the Sun and 65 times the Sun's radius. In all likelihood, it will end its life as a Type II supernova. Omicron2 Canis Majoris is one of the most luminous stars known, as it radiates about 220,000 times as much luminosity as the Sun from its outer envelope at a temperature of 15,500 K. At this heat, the star is glowing with the blue-white hue of a B-type star.
Artist's impression of the dusty torus around WOH G64 (European Southern Observatory) The spectral type of WOH G64 is given as M5, but it is usually found to have a much cooler spectral type of M7.5, highly unusual for a supergiant star. WOH G64 is classified as an extremely luminous M class supergiant and is likely to be the largest star and the most luminous and coolest red supergiant in the LMC. The combination of the star's temperature and luminosity places it toward the upper right corner of the Hertzsprung–Russell diagram. The star's evolved state means that it can no longer hold on to its atmosphere due to low density, high radiation pressure, and the relatively opaque products of thermonuclear fusion.
The fact that ULXs have Eddington luminosities larger than that of stellar mass objects implies that they are different from normal X-ray binaries. There are several models for ULXs, and it is likely that different models apply for different sources. Beamed emission — If the emission of the sources is strongly beamed, the Eddington argument is circumvented twice: first because the actual luminosity of the source is lower than inferred, and second because the accreted gas may come from a different direction than that in which the photons are emitted. Modelling indicates that stellar mass sources may reach luminosities up to 1040 erg/s (1033 W), enough to explain most of the sources, but too low for the most luminous sources.
Deneb spent much of its early life as an O-type main-sequence star of about , but it has now exhausted the hydrogen in its core and expanded to become a supergiant. Stars in the mass range of Deneb eventually expand to become the most luminous red supergiants, and within a few million years their cores will collapse producing a supernova explosion. It is now known that red supergiants up to a certain mass explode as the commonly seen type II-P supernovae, but more massive ones lose their outer layers to become hotter again. Depending on their initial masses and the rate of mass loss, they may explode as yellow hypergiants or luminous blue variables, or they may become Wolf-Rayet stars before exploding in a type Ib or Ic supernova.
No gamma- ray bursts from within our own galaxy, the Milky Way, have been observed, and the question of whether one has ever occurred remains unresolved. In light of evolving understanding of gamma-ray bursts and their progenitors, the scientific literature records a growing number of local, past, and future GRB candidates. Long duration GRBs are related to superluminous supernovae, or hypernovae, and most luminous blue variables (LBVs), and rapidly spinning Wolf–Rayet stars are thought to end their life cycles in core-collapse supernovae with an associated long-duration GRB. Knowledge of GRBs, however, is from metal-poor galaxies of former epochs of the universe's evolution, and it is impossible to directly extrapolate to encompass more evolved galaxies and stellar environments with a higher metallicity, such as the Milky Way.
Closest approach will happen in about 4,000 years, when the star will be a few hundredths of a light-year closer to Earth than it is today. (In antiquity, Arcturus was closer to the centre of the constellation.) Arcturus is thought to be an old-disk star, and appears to be moving with a group of 52 other such stars, known as the Arcturus stream. With an absolute magnitude of −0.30, Arcturus is, together with Vega and Sirius, one of the most luminous stars in the Sun's neighborhood. It is about 110 times brighter than the Sun in visible light wavelengths, but this underestimates its strength as much of the light it gives off is in the infrared; total (bolometric) power output is about 180 times that of the Sun.
St 2-18 shows the traits and properties of a highly luminous and extreme red supergiant, with a late spectral type of M6, which is unusual for a supergiant star. This places it at the top right corner of the Hertzsprung–Russell diagram. A calculation for finding the bolometric luminosity by fitting the Spectral Energy Distribution (SED) gives the star a luminosity of nearly , with an effective temperature of , which corresponds to a very large radius of , which would be considerably larger and more luminous than theoretical models of the largest, and most luminous red supergiants possible (roughly and respectively). An alternate but older calculation from 2010, still assuming membership of the Stephenson 2 cluster at but based on 12 and fluxes, gives a much lower and relatively modest luminosity of .
It is now known that quasars are distant but extremely luminous objects, so any light that reaches the Earth is redshifted due to the metric expansion of space. Quasars inhabit the centers of active galaxies and are among the most luminous, powerful, and energetic objects known in the universe, emitting up to a thousand times the energy output of the Milky Way, which contains 200–400 billion stars. This radiation is emitted across the electromagnetic spectrum, almost uniformly, from X-rays to the far infrared with a peak in the ultraviolet optical bands, with some quasars also being strong sources of radio emission and of gamma-rays. With high-resolution imaging from ground-based telescopes and the Hubble Space Telescope, the "host galaxies" surrounding the quasars have been detected in some cases.
Il pomo d'oro became known all over the world through the prints by Matthäus Küsel and Frans Geffels based on Burnacini's designs. This and other operas, whose libretti were magnificently complimented with large-format engravings, such as Il fuoco eterno delle Vestali (1674) composed by Antonio Draghi and the Monarchia latina trionfante (1678) composed by Draghi and Johann Heinrich Schmelzer vastly contributed to Burnacini's international reputation. In 1688, after a visit to Vienna, the Swedish architect and art collector Nicodemus Tessin the younger wrote: > Bejim H. Burnacini der trusser undt ingegner vom Keijsser ist, habe ich > alles höffligkeit genossen, in theatern undt festen wirdt heüt zu tage dass > gröste lumiere von allen haben. ("At Mr. Burnacini's, who is steward and > engineer of the emperor, I enjoyed all courtesy; concerning theater and > festivities nowadays he will be the most luminous one").
The object is an OVV (optically violent variable) quasar, a type of blazar. It belongs to the most energetic subclass of active galactic nuclei, which are produced by the rapid accretion of matter by a central supermassive black hole, changing gravitational energy to light energy that can be visible at cosmic distances. In the case of S5 0014+81, it is one of the most luminous quasars known, with a total luminosity of over 1041 watts,1.2 × 1041 watts. equal to an absolute bolometric magnitude of −31.5. If the quasar were at a distance of 280 light- years from Earth, it would give out as much energy per square meter as the Sun does at Earth, despite being 18 million times more distant. The quasar's luminosity is therefore about 3 × 1014 (300 trillion) times the Sun,Solar luminosity is 3.846 × 1026 watts.
Active galactic nuclei are the most luminous persistent sources of electromagnetic radiation in the universe, and as such can be used as a means of discovering distant objects; their evolution as a function of cosmic time also puts constraints on models of the cosmos. The observed characteristics of an AGN depend on several properties such as the mass of the central black hole, the rate of gas accretion onto the black hole, the orientation of the accretion disk, the degree of obscuration of the nucleus by dust, and presence or absence of jets. Numerous subclasses of AGN have been defined based on their observed characteristics; the most powerful AGN are classified as quasars. A blazar is an AGN with a jet pointed toward the Earth, in which radiation from the jet is enhanced by relativistic beaming.
Artist's impression of W2246-0526 WISE J224607.57−052635.0 (or W2246−0526 for short) is an extremely luminous infrared galaxy (ELIRG) which, in 2015, was announced as the most luminous known galaxy in the Universe. The brightness is 350 trillion times that of the Sun (349×1012), and the merger of smaller nearby galaxies may be contributing to its brightness. The light is generated by a quasar 10 billion times the mass of the Sun. The optical and ultraviolet light emitted by the accretion disc around the quasar's supermassive black hole is absorbed by the galaxy's dust and remitted in the infrared. The galaxy releases 10,000 times more energy than the Milky Way galaxy, although WISE J224607.57–052635.0 is the smaller of the two. WISE J224607.57–052635.0 has a light-travel distance of 12.5 billion light-years from it to Earth.
The opacity of this ejected hydrogen decreases as it cools and this causes an extended delay to the drop in brightness after the initial supernova peak, the characteristic of a Type II-P supernova. The most luminous red supergiants, at near solar metallicity, are expected to lose most of their outer layers before their cores collapse, hence they evolve back to yellow hypergiants and luminous blue variables. Such stars can explode as type II-L supernovae, still with hydrogen in their spectra but not with sufficient hydrogen to cause an extended brightness plateau in their light curves. Stars with even less hydrogen remaining may produce the uncommon type IIb supernova, where there is so little hydrogen remaining that the hydrogen lines in the initial type II spectrum fade to the appearance of a Type Ib supernova.
Betelgeuse (Alpha Orionis) is a bright red star in the constellation Orion frequently featured in works of science fiction. A red supergiant, Betelgeuse is one of the largest and most luminous stars known. If it were at the center of our Solar System its surface would extend past the asteroid belt, possibly to the orbit of Jupiter or even beyond, wholly engulfing Mercury, Venus, Earth and Mars. Classified as an M-type supergiant star, and located around 640 light- years from Earth, Betelgeuse shares with the much closer but smaller star Altair (and with R Doradus) the distinction that its image has been resolved by astronomers (see graphic The yellowish red "image" or "photo" of Betelgeuse usually seen is actually not a picture of the red giant but rather a mathematically generated image based on the photograph.
The spectral type of MY Cephei is given in the General Catalogue of Variable Stars as M6–7 Iab, indicating the star is an intermediate-size luminous supergiant star, although most authors gives M7–M7.5 I. Classification is difficult because of the lack of comparable standard stars, but its spectrum appears to be later than M5, earlier than VX Sagittarii when at M9, and more luminous than M7 giant stars. MY Cephei is a very luminous, cool and large extreme supergiant star, with a luminosity more than 100,000 times that of the Sun () and a radius in excess of a thousand times the Sun's radius (). It is likely the most luminous, coolest, and the largest supergiant star in its open cluster, and occupies the upper-right hand corner of the Hertzsprung–Russell diagram. A 2018 paper gives the star a temperature of , corresponding a radius of based on a luminosity of .
Artist's conception showing the relative sizes of the Sun (Sol) and blue supergiant Rigel, 71 times larger. Rigel (Beta Orionis) is a luminous blue supergiant of spectral type B8 Iae, in the constellation Orion. The star is actually a visual binary, with the secondary component Rigel B itself being a spectroscopic binary that has never been resolved visually, and which taken as a single source is 500 times dimmer and over 2200 AU from its overwhelming companion Rigel A ("Rigel"). This irregular variable star is the most luminous in our local region of the Milky Way; at about 71 times the diameter of the Sun it would, if viewed from a hypothetical planet at a distance of 1 AU, subtend an angle of 35° in the sky—when rising or setting it would extend from the horizon almost halfway up the sky—and it would shine at a lethal magnitude of −38 (see graphic).
The 1996 New York debut of the Nrityagram Dance Ensemble, with Surupa Sen, Bijayini Satpathy, Anitha Nair, Pavithra Reddy and Jaya Mukherjee was called, "one of the most luminous dance events of the year" by Jennifer Dunning, the dance critic of the New York Times. After its New York debut, the Nrityagram Dance Ensemble has performed to sold-out shows in Hawai and Bozeman, USA, Middle East, Far East and Europe, and in time created a niche for itself in the world of dance. Today, apart from lead dancer-choreographers, Surupa Sen and Bijayini Satpathy, Pavitra Reddy, Rasmi Raj and Manasi Tripathy are the other permanent dancers of the Ensemble, and are accompanied by musicians like Swain playing the percussion instrument, Mardala, Srinibas Satapathy’s on Bamboo flute (Bansuri) and Sanjib Kumar Kunda on the violin. Its first full- length production "Sri - In Search of the Goddess", was premiered in Delhi in 2001 and in the United States in 2002-2003, to critical acclaim.
Despite being one of the most luminous stars known, 500,000 times brighter than the Sun, IRC+10420 cannot be seen with the naked eye and needs a telescope to be observed. IRC+10420's spectrum has changed from late F to early A in recent decades without experiencing changes in its luminosity. This suggests IRC+10420 is a former red supergiant that is evolving blueward on the Hertzsprung-Russell diagram to become a luminous blue variable, or Wolf–Rayet star. Models suggest it started its life as a 40-50 solar masses star that lost most of its mass due to strong stellar winds leaving it with just 10 solar masses and that the star - which actually has a high surface temperature - is totally enshrouded in the matter it has expelled appearing as a fake photosphere, so IRC+10420 appears with a later spectral type as humans see just the expelled dust and gas it has blown out during its life and not the star itself.
In one of these, on the political economy of Adam Smith, he exhibits in a very interesting way the co-existence in The Wealth of Nations of historical-inductive investigation in the manner of Montesquieu with a priori speculation founded on theologico-metaphysical bases, and points out the error of ignoring the former element, which is the really characteristic feature of Smith's social philosophy, and places him in strong contrast with the school of Ricardo. The essay, however, which contains the most brilliant polemic against the orthodox school, as well as the most luminous account and the most powerful vindication of the new direction, was that of which we have above spoken as having first appeared in Hermathena. "On the Philosophical Method of Political Economy", Hermathena, Dublin University (1876) It may be recommended as supplying the best extant presentation of one of the two contending views of economic method. On this essay mainly rests the claim of Leslie to be regarded as the founder and first head of the English historical school of political economy.

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