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Aldebaran - Wikipedia, the free encyclopedia. Aldebaran. Observation data. Epoch. J2. 00. 0.
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Equinox. J2. 00. 0. Constellation. Taurus. Pronunciation. It is the brightest star in its constellation and usually the fourteenth brightest star in the nighttime sky, though it varies slowly in brightness between magnitude 0.
It is likely that Aldebaran hosts a planet several times the size of Jupiter. The planetary exploration probe Pioneer 1. The name Aldebaran is Arabic (. The WGSN's first bulletin of July 2. It is now so entered in the IAU Catalog of Star Names. It has three names: Hant Caalajc Ip.
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The lunar month corresponding to October is called Queeto yaao . The woman's husband tracked him down and burned the tree in which he was hiding. It is believed that he rose to the sky as smoke and became the star Aldebaran. This, as well as observations of the changing positions of stars Sirius and Arcturus, led to the discovery of proper motion.
Based on present day observations, the position of Aldebaran has shifted 7. This star was shown to be itself a close double star by S. Burnham in 1. 88. Follow on measurements of proper motion showed that Herschel's companion was diverging from Aldebaran, and hence they were not physically connected. However, the companion discovered by Burnham had almost exactly the same proper motion as Aldebaran, suggesting that the two formed a wide binary star system. Pickering at the Harvard College Observatory used a photographic plate to capture fifty absorption lines in the spectrum of Aldebaran.
This became part of the Draper Catalogue, published in 1. By 1. 88. 7, the photographic technique had improved to the point that it was possible to measure a star's radial velocity from the amount of Doppler shift in the spectrum. By this means, the recession velocity of Aldebaran was estimated as 3.
Potsdam Observatory by Hermann C. Vogel and his assistant Julius Scheiner.
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The result was 0. The collapse of the centre of the star into a degenerate helium core has ignited a shell of hydrogen outside the core and Aldebaran is now a red giant. Aldebaran is a slightly variable star, of the slow irregular variable type LB. It varies by about 0. However, small scale magnetic fields may still be present in the lower atmosphere, resulting from convection turbulence near the surface. This region lies between 1. The spectrum reveals lines of carbon monoxide, water, and titanium oxide.
The wind continues to expand until it reaches the termination shock boundary with the hot, ionized interstellar medium that dominates the Local Bubble, forming a roughly spherical astrosphere with a radius of around 1,0. AU, centered on Aldebaran. If one follows the three stars of Orion's belt from left to right (in the Northern Hemisphere) or right to left (in the Southern), the first bright star found by continuing that line is Aldebaran. Since the star is located (by chance) in the line of sight between the Earth and the Hyades, it has the appearance of being the brightest member of the more scattered Hyadesopen star cluster that makes up the bull's- head- shaped asterism; however, the star cluster is actually more than twice as far away, at about 1. Aldebaran is close enough to the ecliptic to be occulted by the Moon. Such occultations occur when the Moon's ascending node is near the autumnal equinox. A series of 4. 9 occultations occur starting at 2.
Jan 2. 01. 5 and ending at 3 Sep 2. That means that people in e. Australia or South Africa can never observe an Aldebaran occultation. This is due to the fact that Aldebaran is slightly too far south of the ecliptic. A reasonably accurate estimate for the diameter of Aldebaran was obtained during the September 2.
These double stars were given alphabetic secondary star designations more or less in the order of their discovery, with the letter A reserved for the primary star. Some of the characteristics of these components, including their position relative to Aldebaran, are listed in the table at right. Some surveys have indicated that Alpha Tauri B may have about the same proper motion and parallax as Aldebaran and thus may be a physical binary system. However these measurements are difficult to make because the dim B component appears so close to the bright primary star. The resulting margin of error is too large to positively establish (or exclude) a physical relationship between the two stars. So far neither the B component, nor anything else, has been unambiguously shown to be physically associated with Aldebaran. These co- orbiting stars have been shown to be located far beyond Aldebaran and are members of the Hyades star cluster.
As with the rest of the stars in the cluster they do not physically interact with Aldebaran in any way. The measurements for Aldebaran implied a companion with a minimum mass 1. Jupiter in a 6. 43- day orbit at a separation of 2. AU (3. 00 Gm) in a mildly eccentric orbit. However, all three stars surveyed showed similar oscillations yielding similar companion masses, and the authors concluded that the variation was likely to be intrinsic to the star rather than due to the gravitational effect of a companion. Astronomy and Astrophysics. Bibcode: 2. 00. 7A& A..
V. CDS/ADC Collection of Electronic Catalogues. Bibcode: 2. 00. 2y. Cat. 2. 23. 7.. 0. D. General Catalogue of Variable Stars. The Astronomical Journal.
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