33 Sentences With "solar prominences" | Random Sentence Generator

In addition to eclipses, he painted solar prominences, views from other planets, and the lunar surface.

We'll also pass through the chromosphere and photosphere, where we might get a glimpse of sunspots, solar prominences, and solar flares.

The spacecraft is responsible for creating some of the highest resolution photos of solar flares, coronal holes and solar prominences emanating from the star.

Its announcers plan to have a solar physicist nearby to explain the plasma activity the crowd may potentially see, like sunspots, solar prominences and coronal mass ejections.

The result of emerging twisted flux tubes from the interior of the sun cause twisted magnetic structures in the corona, which then lead to solar prominences. Solar prominences are modeled using twisted magnetic flux tubes known as flux ropes.

H-alpha light is the brightest hydrogen line in the visible spectral range. It is important to astronomers as it is emitted by many emission nebulae and can be used to observe features in the Sun's atmosphere, including solar prominences and the chromosphere.

The Sun was photographed for the first time, on 2 April 1845, by French physicists Louis Fizeau and Léon Foucault. Sunspots, as well as the limb darkening effect, are visible in their daguerrotypes. Photography assisted in the study of solar prominences, granulation and spectroscopy. Charles A. Young first captured a prominence in 1870.

Solar storms of different types are caused by disturbances on the Sun, most often coronal clouds associated with coronal mass ejections (CMEs) produced by solar flares emanating from active sunspot regions, or, less often, from coronal holes. Solar filaments (solar prominences) may also trigger CMEs, trigger flares, or occur in conjunction with flares, and the associated CMEs can be intensified.

Therese "Terry" Kucera is an astrophysicist in NASA Goddard Space Flight Center's Solar Physics Laboratory. Her research interests center on the solar atmosphere, especially solar prominences and prominence cavities. She currently serves as Project Scientist for NASA's STEREO project. Dr. Kucera came to NASA/Goddard in 1993 after receiving her doctorate from the University of Colorado, Boulder, where she studied radio emissions from solar flares.

Solar prominences observed by Carl Frederik Fearnley during solar cycle 11 (1872–1873). Solar cycle 11 was the eleventh solar cycle since 1755, when extensive recording of solar sunspot activity began. The solar cycle lasted 11.8 years, beginning in March 1867 and ending in December 1878. The maximum smoothed sunspot number observed during the solar cycle was 234.0 (August 1870), and the starting minimum was 9.9.

Solar prominences during an eclipse in solar cycle 13 (28 May 1900). Solar cycle 13 was the thirteenth solar cycle since 1755, when extensive recording of solar sunspot activity began. The solar cycle lasted 11.8 years, beginning in March 1890 and ending in January 1902. The maximum smoothed sunspot number (SIDC formula) observed during the solar cycle was 146.5 (January 1894), and the starting minimum was 8.3.

Solar spectroscopy began in the 1800s, from which properties of the solar atmosphere could be determined, while the creation of daguerreotypy led to the first solar photographs on 2 April 1845. Photography assisted in the study of solar prominences, granulation and spectroscopy. Early in the 20th century, interest in astrophysics surged in America. A number of new observatories were built with solar telescopes around the world.

Beginning in 1941, when he attended a lecture on astrophysics at Edinburgh University, Bruce's own interests headed in the same direction. He immediately developed a theory that solar prominences consisted of electrical discharges in plasma, rather than of moving solar matter, and he eventually published over 100 papers concerning the electrical basis of various cosmological phenomena. However, his work in this area has been largely ignored by mainstream science.

Totality during the 1999 solar eclipse. Solar prominences can be seen along the limb (in red) as well as extensive coronal filaments. An eclipse is an astronomical event that occurs when an astronomical object or spacecraft is temporarily obscured, by passing into the shadow of another body or by having another body pass between it and the viewer. This alignment of three celestial objects is known as a syzygy.

Solar prominences during solar cycle 14 (21 August 1909). Solar cycle 14 was the fourteenth solar cycle since 1755, when extensive recording of solar sunspot activity began. The solar cycle lasted 11.5 years, beginning in January 1902 and ending in July 1913. The maximum smoothed sunspot number (SIDC formula) observed during the solar cycle was 107.1, in February 1906 (the lowest since the Dalton Minimum), and the starting minimum was 4.5.

Coronal loops — linking areas of opposite magnetic polarity in the photosphere — enormous solar prominences and sunspots are all to be seen here. Coronal loops are huge loops of magnetic field beginning and ending on the Sun's visible surface (photosphere) projecting into the solar atmosphere (corona). Hot glowing ionized gas (plasma) trapped in the loops makes them visible. Coronal loops range widely in size up to several thousand kilometers long.

He wrote of the 22 December 968 total eclipse, which he experienced in Constantinople (modern-day Istanbul, Turkey): alt=Black and white drawing showing Latin script surrounding two concentric circles with two black dots inside the inner circle The earliest known record of a sunspot drawing was in 1128, by John of Worcester. Another early observation was of solar prominences, described in 1185 in the Russian Chronicle of Novgorod.

After completing his studies in 1878, he would return to teaching and also serve as an assistant at the Haynald Observatory in Kalocsa. In 1885 he became the director of the observatory, and would remain at this post until retiring due to poor health in 1913. He continued his astronomical observations even in retirement. Fényi Gyula was noted for his observations of the Sun, including spectroscopic studies of solar prominences, as well as sun spots.

He was the first person to demonstrate a correlation between the number of solar prominences and the number of sun spots. Between 1880 until 1919 he assembled over 6,000 drawings of the Sun, all using the same instrument. (These drawings are archived at the Heliophysical Observatory, in Debrecen, Hungary.) He published over 200 scientific papers in several languages. In 1916 he was elected a corresponding member of the Hungarian Academy of Sciences.

Accompanying solar flares or large solar prominences, "coronal transients" (also called coronal mass ejections) are sometimes released. These are enormous loops of coronal material that travel outward from the Sun at over a million kilometers per hour, containing roughly 10 times the energy of the solar flare or prominence that accompanies them. Some larger ejections can propel hundreds of millions of tons of material into space at roughly 1.5 million kilometers an hour.

Through the early 1990s spheromak work was widely used by the astrophysics community to explain various events and the spheromak was studied as an add-on to existing MFE devices. D.M. Rust and A. Kumar were particularly active in using magnetic helicity and relaxation to study solar prominences."Publications for the years" Similar work was carried out at Caltech by Bellan and Hansen at Caltech, and the Swarthmore Spheromak Experiment (SSX) project at Swarthmore College.

Solar prominences observed by Carl Frederik Fearnley in 1872-73 Carl Frederik Fearnley (born 19 December 1818 in Frederikshald, died 22 August 1890 in Christiania) was a Norwegian astronomer and Professor at the Royal Frederick University. He was the brother of romantic painter Thomas Fearnley. Fearnley was the son of merchant Thomas Fearnley (1768–1834) and Maren Sophie Paus (1782–1838). He graduated in mineralogy in 1844, and became an observer at the Royal Frederick University Observatory the same year.

This instrument was designed to take motion pictures of the Sun. The McMath-Hulbert Solar Observatory is primarily known for the motion pictures that the McMaths made of various celestial phenomena, including the first movies of solar prominences in motion. Later work involved solar spectroscopy in the near infrared and participation in a solar flare patrol program in the 1950s. Robert McMath and one of the resident astronomers, Keith Pierce, established the McMath-Pierce Solar Telescope at Kitt Peak Observatory near Tucson, Arizona in 1962.

Pedler was the son of George Standbury, a pharmacist on Fleet Street, and Hannah Rideal. He was privately schooled and educated at the City of London School. With a Bell scholarship he studied at the laboratory of the Pharmaceutical Society of Great Britain from 1866. He worked as a chemical assistant at the Royal Institution, working with Herbert McLeod, Edward Frankland, and Norman Lockyer. He worked with Lockyer examining the spectra from solar prominences in Sicily when the latter discovered helium on the earth in 1868.

In 1868 Janssen discovered how to observe solar prominences without an eclipse. While observing the solar eclipse of 18 August 1868, at Guntur, Madras State (now in Andhra Pradesh), British India, he noticed bright lines in the spectrum of the chromosphere, showing that the chromosphere is gaseous. Present in the spectrum of the Sun, though not immediately noticed or commented upon, was a bright yellow line later measured to have a wavelength of 587.49 nm. This was the first observation of this particular spectral line, and one possible source for it was an element not yet discovered on the earth.

French astronomer Pierre Janssen observed the eclipse from Guntur in Madras State, British India. It was the first total eclipse since Gustav Kirchhoff's 1859 theory that the Fraunhofer lines in the solar spectrum correspond to the emission line of the different chemical elements present in the Sun. Correspondingly, Janssen observed the eclipse with the aid of a spectroscope. He noticed a bright yellow line (λ = 587.49 nm) in the spectra of the solar prominences that could not be due to sodium as had previously been assumed, and was subsequently able to observe the same line even without the need for an eclipse.

Add-ons also include space objects such as red and blue supergiants, red and brown dwarfs, neutron stars, spinning pulsars, rotating black holes with accretion disks, protostars, star nursery nebulae, supernova remnants, planetary nebulae, galactic redshifts, geological planetary displays (e.g. 3D interiors, topographic and bathymetric maps, paleogeography), planetary aurorae, rotating magnetic fields, animated solar prominences, 3D craters and mountains, and historic collision events. Numerous scripts are available. These include simple tours, reconstructions of complex space missions such as Cassini–Huygens and Deep Impact, and scripts showing useful information, like size comparisons, or particular events such as multiple simultaneous eclipses of Jupiter's moons or the evolution of a star.

Active regions are ensembles of loop structures connecting points of opposite magnetic polarity in the photosphere, the so-called coronal loops. They generally distribute in two zones of activity, which are parallel to the solar equator. The average temperature is between two and four million kelvin, while the density goes from 109 to 1010 particles per cm3. Illustration depicting solar prominences and sunspots Active regions involve all the phenomena directly linked to the magnetic field, which occur at different heights above the Sun's surface: sunspots and faculae, occur in the photosphere, spicules, Hα filaments and plages in the chromosphere, prominences in the chromosphere and transition region, and flares and coronal mass ejections happen in the corona and chromosphere.

According to the Lay, after the eclipse Igor gave a long speech to his retinue to allay their fears before proceeding on his campaign. The eclipse is mentioned in the 14th-century Laurentian Chronicle with the first detailed description of solar prominences. They were described as flame-like tongues of live embers: > On the first day of the month of May, on the day of the Saint Prophet > Jeremiah, on Wednesday, during the evening service, there was a sign in the > Sun. It became very dark, even the stars could be seen; it seemed to men as > if everything were green, and the Sun became like a crescent of the Moon, > from the horns of which a glow similar to that of red-hot charcoals was > emanating.

In 1917, James Hopwood Jeans argued that only a very close approach of a second star was necessary to eject material, instead of requiring solar prominences. In 1939, Lyman Spitzer showed that a column of material drawn out from the sun would dissipate rather than condense. By this time the theory had mostly fallen out of favor, and in the 1940s, the work of Henry Norris Russell showed that if the solar material had been pulled away from the sun with the force necessary to account for the angular momentum of Jupiter, the material would have continued out of the solar system entirely. Though the Chamberlin–Moulton hypothesis is no longer accepted, the idea of planetesimals remains in modern theory.

Moulton and Chamberlin suggested that a star had passed close to the Sun early in its life to cause tidal bulges and that this, along with the internal process that leads to solar prominences, resulted in the ejection of filaments of matter from both stars. While most of the material would have fallen back, part of it would remain in orbit. The filaments cooled into numerous, tiny, solid fragments, ‘planetesimals’, and a few larger protoplanets. This model received favourable support for about 3 decades but passed out of favour by the late '30s and was discarded in the '40s by the realization it was incompatible with the angular momentum of Jupiter, but a part of it, planetesimal accretion, was retained.

The Chamberlin–Moulton planetesimal hypothesis was proposed in 1905 by geologist Thomas Chrowder Chamberlin and astronomer Forest Ray Moulton to describe the formation of the Solar System. It was proposed as a replacement for the Laplacian version of the nebular hypothesis that had prevailed since the 19th century. The hypothesis was based on the idea that a star passed close enough to the sun early in its life to cause tidal bulges to form on its surface, which along with the internal process that leads to solar prominences, caused material to be ejected repeatedly from the sun. Due to the gravitational effects of the passing star, two spiral-like arms would have extended from the sun, and while most of the material would have fallen back, part of it would remain in orbit.

He speculates that the obviously missing visors were perhaps not noticed until late in the filming and that a scene which explains the ray screens was inserted prior to the film's release, before audiences could wonder about it. Bryan Senn, also an American critic, notes that "The effects are minimal and substandard, consisting mainly of the same shot of a rocket traveling through space used over and over again (and it's not even a convincing shot - the stars shine right through the transparent-looking ship)", although he calls the Moon set "eerie and effectively alien, with its cracks, weird shadows, and smoke seeping from mysterious holes". Warren points out that the Earth-saving eruption of Popocatepetl is "depicted by stock footage of solar prominences" that bear little resemblance to real volcanic eruptions. Modern critics are also bothered by the narrative development of the film.