Aldebaran /ælˈdɛbərən/, designated α Tauri (Latinized to Alpha Tauri, abbreviated Alpha Tau, α Tau), is a giant star measured to be about 65 light-years from the Sun in the zodiac constellation Taurus. It is the brightest star in Taurus and generally the fourteenth-brightest star in the night sky, though it varies slowly in brightness between magnitude 0.75 and 0.95. Aldebaran is believed to host a planet several times the mass of Jupiter, named Aldebaran b.
Aldebaran is a giant star, cooler than the sun with a surface temperature of 3,900 K, but its radius is about 44 times the sun's, so it is over 400 times as luminous. It spins slowly and takes 520 days to complete a rotation.
The planetary exploration probe Pioneer 10 is heading in the general direction of the star and should make its closest approach in about two million years.
Nomenclature
Aldebaran is the brightest star in the constellation of Taurus (center).
The traditional name Aldebaran derives from the Arabic al Dabarān ("الدبران"), meaning "the follower", because it seems to follow the Pleiades.[16][17] In 2016, the International Astronomical Union Working Group on Star Names (WGSN) approved the proper name Aldebaran for this star.[18][19]
Aldebaran is the brightest star in the constellation Taurus and so has the Bayer designation α Tauri, Latinised as Alpha Tauri. It has the Flamsteed designation 87 Tauri as the 87th star in the constellation of approximately 7th magnitude or brighter, ordered by right ascension. It also has the Bright Star Catalogue number 1457, the HD number 29139, and the Hipparcos catalogue number 21421, mostly seen in scientific publications.
It is a variable star listed in the General Catalogue of Variable Stars, but it is listed using its Bayer designation and does not have a separate variable star designation.[4]
Aldebaran and several nearby stars are included in double star catalogues such as the Washington Double Star Catalog as WDS 04359+1631 and the Aitken Double Star Catalogue as ADS 3321. It was included with an 11th-magnitude companion as a double star as H IV 66 in the Herschel Catalogue of Double Stars and Σ II 2 in the Struve Double Star Catalog, and together with a 14th-magnitude star as β 550 in the Burnham Double Star Catalogue.[20][21]
Observation
Aldebaran in the Hyades
Aldebaran is one of the easiest stars to find in the night sky, partly due to its brightness and partly due to being near one of the more noticeable asterisms in the sky. Following the three stars of Orion's belt in the opposite direction to Sirius, the first bright star encountered is Aldebaran.[22]
The star is, by chance, in the line of sight between the Earth and the Hyades, so it has the appearance of being the brightest member of the open cluster, but the cluster that forms the bull's-head-shaped asterism is more than twice as far away, at about 150 light years.[23]
Aldebaran is 5.47 degrees south of the ecliptic and so can be occulted by the Moon. Such occultations occur when the Moon's ascending node is near the autumnal equinox.[24] A series of 49 occultations occurred starting on 29 January 2015 and ending at 3 September 2018.[25] Each event was visible from points in the northern hemisphere or close to the equator; people in e.g. Australia or South Africa can never observe an Aldebaran occultation since it is too far south of the ecliptic. A reasonably accurate estimate for the diameter of Aldebaran was obtained during the occultation of 22 September 1978.[26] Aldebaran is in conjunction with the Sun around June 1 of each year.[27]
With a near-infrared J band magnitude of −2.1, only Betelgeuse (−2.9), R Doradus (−2.6), and Arcturus (−2.2) are brighter at that wavelength.[7]
Observational history
Occultation of Aldebaran by the Moon. Aldebaran is the red dot to the right, barely visible in the thumbnail.
On 11 March AD 509, a lunar occultation of Aldebaran was observed in Athens, Greece.[28] English astronomer Edmund Halley studied the timing of this event, and in 1718 concluded that Aldebaran must have changed position since that time, moving several minutes of arc further to the north. 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′ in the last 2000 years; roughly a quarter the diameter of the full moon.[29][30] Due to precession of the equinoxes, 5,000 years ago the equinox (Northern Hemisphere)|vernal equinox was close to Aldebaran.[31]
English astronomer William Herschel discovered a faint companion to Aldebaran in 1782;[32] an 11th-magnitude star at an angular separation of 117″. This star was shown to be itself a close double star by S. W. Burnham in 1888, and he discovered an additional 14th-magnitude companion at an angular separation of 31″. 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.[33]
Working at his private observatory in Tulse Hill, England, in 1864 William Huggins performed the first studies of the spectrum of Aldebaran, where he was able to identify the lines of nine elements, including iron, sodium, calcium, and magnesium. In 1886, Edward C. 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 1890. By 1887, 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 30 miles per second (48 km/s), using measurements performed at Potsdam Observatory by Hermann C. Vogel and his assistant Julius Scheiner.[34]
Aldebaran was observed using an interferometer attached to the Hooker Telescope at the Mount Wilson Observatory in 1921 in order to measure its angular diameter, but it was not resolved in these observations.[35]
The extensive history of observations of Aldebaran led to it being included in the list of 33 stars chosen as benchmarks for the Gaia mission to calibrate derived stellar parameters.[36] It had previously been used to calibrate instruments on board the Hubble Space Telescope.[13]
Physical characteristics
Size comparison between Aldebaran and the Sun
Aldebaran is listed as the spectral standard for type K5+ III stars.[6] Its spectrum shows that it is a giant star that has evolved off the main sequence band of the Hertzsprung–Russell diagram after exhausting the hydrogen at its core. 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 on the red giant branch (RGB).[5]
The effective temperature of Aldebaran's photosphere is 3,910 K. It has a surface gravity of 1.59 cgs, typical for a giant star, but around 25 times lower than the Earth's and 700 times lower than the sun's. Its metallicity is about 30% lower than the sun's.
Measurements by the Hipparcos satellite and other sources put Aldebaran around 65.3 light-years (20.0 parsecs) away.[10] Asteroseismology has determined that it is about 16% more massive than the Sun,[11] yet it shines with 518 times the Sun's luminosity due to the expanded radius. The angular diameter of Aldebaran has been measured many times. The value adopted as part of the Gaia benchmark calibration is 20.580±0.030 mas.[13] It is 44 times the diameter of the Sun, approximately 61 million kilometres.[12]
Aldebaran is a slightly variable star, assigned to the slow irregular type LB. The General Catalogue of Variable Stars indicates variation between apparent magnitude 0.75 and 0.95 from historical reports.[4] Modern studies show a smaller amplitude, with some showing almost no variation.[37] Hipparcos photometry shows an amplitude of only about 0.02 magnitudes and a possible period around 18 days.[38] Intensive ground-based photometry showed variations of up to 0.03 magnitudes and a possible period around 91 days.[37] Analysis of observations over a much longer period still find a total amplitude likely to be less than 0.1 magnitudes, and the variation is considered to be irregular.[39]
The photosphere shows abundances of carbon, oxygen, and nitrogen that suggest the giant has gone through its first dredge-up stage—a normal step in the evolution of a star into a red giant during which material from deep within the star is brought up to the surface by convection.[40] With its slow rotation, Aldebaran lacks a dynamo needed to generate a corona and hence is not a source of hard X-ray emission. However, small scale magnetic fields may still be present in the lower atmosphere, resulting from convection turbulence near the surface. The measured strength of the magnetic field on Aldebaran is 0.22 Gauss.[41] Any resulting soft X-ray emissions from this region may be attenuated by the chromosphere, although ultraviolet emission has been detected in the spectrum.[42] The star is currently losing mass at a rate of (1–1.6) × 10−11 M⊙ yr−1 (about one Earth mass in 300,000 years) with a velocity of 30 km s−1.[40] This stellar wind may be generated by the weak magnetic fields in the lower atmosphere.[42]
Beyond the chromosphere of Aldebaran is an extended molecular outer atmosphere (MOLsphere) where the temperature is cool enough for molecules of gas to form. This region lies at about 2.5 times the radius of the star and has a temperature of about 1,500 K. The spectrum reveals lines of carbon monoxide, water, and titanium oxide.[40] Outside the MOLSphere, the stellar 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 1,000 AU, centered on Aldebaran.[43]
Visual companions
Five faint stars appear close to Aldebaran in the sky. These double star components were given upper-case Latin letter designations more or less in the order of their discovery, with the letter A reserved for the primary star. Some characteristics of these components, including their position relative to Aldebaran, are shown in the table.
WDS 04359+1631 Catalogue Entry[21] α Tau Apparent
Magnitude Angular
Separation (″) Position
Angle (°) Year Parallax (mas)
B 13.60 31.60 113 2007 47.3417±0.1055[44]
C 11.30 129.50 32 2011 19.1267±0.4274[45]
D 13.70 — — — —
E 12.00 36.10 323 2000
F 13.60 255.70 121 2000 0.1626±0.0369[46]
Some surveys, for example Gaia Data Release 2,[44] 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. These measurements are difficult, since the dim B component appears so close to the bright primary star, and the margin of error is too large to establish (or exclude) a physical relationship between the two. So far neither the B component, nor anything else, has been unambiguously shown to be physically associated with Aldebaran.[47] A spectral type of M2.5 has been published for Alpha Tauri B.[48]
Alpha Tauri CD is a binary system with the C and D component stars gravitationally bound to and co-orbiting each other. 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.[32]
Planetary system
Main article: Aldebaran b
In 1993 radial velocity measurements of Aldebaran, Arcturus and Pollux showed that Aldebaran exhibited a long-period radial velocity oscillation, which could be interpreted as a substellar companion. The measurements for Aldebaran implied a companion with a minimum mass 11.4 times that of Jupiter in a 643-day orbit at a separation of 2.0 AU (300 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.[49]
Big dipper as seen from Aldebaran
In 2015 a study showed stable long-term evidence for both a planetary companion and stellar activity.[15] An asteroseismic analysis of the residuals to the planet fit has determined that Aldebaran b has a minimum mass of 5.8±0.7 Jupiter masses, and that when the star was on the main sequence it would have given this planet Earth-like levels of illumination and therefore, potentially, temperature.[11] This would place it and any of its moons in the habitable zone.
Etymology and mythology
Aldebaran was originally نير الضبران (Nā᾽ir al Dabarān in Arabic), meaning "the bright one of the follower". al Dabarān (الدبران) then applied to the whole of the lunar mansion containing the Hyades.[17] It is assumed that what it was following is the Pleiades.[16] A variety of transliterated spellings have been used, with the current Aldebaran becoming standard relatively recently.[17]
Mythology
This easily seen and striking star in its suggestive asterism is a popular subject for ancient and modern myths.
Mexican culture: For the Seris of northwestern Mexico, this star provides light for the seven women giving birth (Pleiades). It has three names: Hant Caalajc Ipápjö, Queeto, and Azoj Yeen oo Caap ("star that goes ahead"). The lunar month corresponding to October is called Queeto yaao "Aldebaran's path".[50]
Aboriginal culture: in the Clarence River of northeastern New South Wales, this star is the Ancestor Karambal, who stole another man's wife. 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.[51]
Names in other languages
In Hindu astronomy it is identified as the lunar mansion Rohini ("the red one") and as one of the twenty-seven daughters of Daksha and the wife of the god Chandra (Moon).
In Ancient Greek it has been called Λαμπαδίας Lampadias, literally "torch-like or -bearer".[52]
In Chinese, 畢宿 (Bì Xiù), meaning Net, refers to an asterism consisting Aldebaran, ε Tauri, δ3 Tauri, δ1 Tauri, γ Tauri, 71 Tauri and λ Tauri.[53] Consequently, the Chinese name for Aldebaran itself is 畢宿五 (Bì Xiù wǔ), "the Fifth Star of Net".[54]
In modern culture
Italian frigate F590 Aldebaran
The name Aldebaran or Alpha Tauri has been adopted many times, including
Aldebaran Rock in Antarctica
United States Navy stores ship USS Aldebaran (AF-10) and Italian frigate Aldebaran (F 590)
proposed micro-satellite launch vehicle Aldebaran
French company Aldebaran Robotics
fashion brand AlphaTauri
Formula 1 team Scuderia AlphaTauri, previously known as Toro Rosso
The star also appears in works of fiction such as Far From the Madding Crowd and Down and Out in Paris and London. It is frequently seen in science fiction, including the Lensman series and Fallen Dragon. As the brightest star in a Zodiac constellation, it is also given great significance within astrology.
Aldebaran regularly features in conspiracy theories as one of the origins of extraterrestrial aliens,[55] often linked to Nazi UFOs.[56] A well-known example is the German conspiracy theorist Axel Stoll, who considered the star the home of the Aryan race and the target of expeditions by the Wehrmacht.[57]
The planetary exploration probe Pioneer 10 is no longer powered or in contact with Earth, but its trajectory is taking it in the general direction of Aldebaran. It is expected to make its closest approach in about two million years.[58]
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External links
Wikimedia Commons has media related to Aldebaran.
"Aldebaran 2". SolStation. Archived from the original on 25 November 2005. Retrieved 14 November 2005.
Daytime occultation of Aldebaran by the Moon (Moscow, Russia) YouTube video
Coordinates: Sky map 04h 35m 55.2s, +16° 30′ 33″
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Stars of Taurus
Bayer
α (Aldebaran) β (Elnath) γ (Prima Hyadum) δ1 (Secunda Hyadum) δ2 δ3 ε (Ain) ζ (Tianguan) η (Alcyone) θ1 θ2 ι κ1 κ2 λ μ ν ξ ο π ρ σ1 σ2 τ υ φ χ ψ ω1 ω2
Flamsteed
4 (s) 5 (f) 6 (t) 7 9 10 11 12 13 14 16 (Celaeno) 17 (Electra) 18 19 (Taygeta) 20 (Maia) 21 (Asterope) 22 (Asterope II) 23 (Merope) 24 26 27 (Atlas) 28 (Pleione) 29 (u) 30 (e) 31 32 33 36 37 (A1) 39 (A2) 40 41 44 (p) 45 46 47 48 51 53 55 56 57 (h) 58 60 62 63 66 (r) 70 71 72 75 76 79 (b) 80 81 83 84 85 88 (d) 89 90 (c) 93 95 96 97 (i) 98 (k) 99 101 103 104 (m) 105 106 (i) 107 108 109 (n) 110 111 113 114 (o) 115 116 117 118 119 120 121 122 125 126 127 128 129 130 131 132 133 134 135 136 137 139 140 44 Eri 49 Eri
Variable
T Y Z RR RV RW RY RZ SU SV SZ TU UX UZ VY XX XZ AA AH BP CD CI CQ CT CU CW CY DD DF DG DH DI DL DM DN DO DQ DR DS EQ EU FN FS FU FV GG GI GK GV HK HL HU IK V410 V471 V473 V479 V534 V624 V647 V650 V710 V711 V731 V766 V773 V774 V781 V807 V818 V819 V826 V827 V827 V830 V833 V834 V836 V837 V892 V987 V1038 V1062 V1116 V1137 V1141 V1143 V1156 V1187 V1229 V1232 V1241 (WX Eri) V1298
HR
1023 1028 1039 1067 1085 1089 1102 1103 1110 1119 1137 1159 1172 1183 1185 1188 1201 1222 1224 1233 1237 1238 1253 1254 1257 1279 1280 1284 1295 1307 1310 1315 1349 1354 1358 1360 1370 1385 1400 1402 1403 1406 1413 1425 1427 1436 1442 1445 1446 1448 1455 1477 1480 1490 1512 1517 1554 1566 1575 1585 1633 1642 1741 1750 1755 1831 1847 1860 1878 1902 1921 1929 1954 1997 2013 2074
HD
21032 21585 23514 23712 24040 24368 24496 26292 27860 28086 28375 28678 29627 29647 36112 37124 38263 38524 285507
Gliese
Gliese 176
Other
2MASS J03552337+1133437 2MASS J04070752+1546457 2MASS J04414489+2301513 A0535+26 BD +24 692 Butterfly star CoKu Tau/4 Crab Pulsar Elias 16 Elias 18 GD 71 Haro 6-37 HBC 379 HH 30 HII 686 HII 1306 HII 1883 HII 3163 HL Tau 76 HP Tau/G2 Hubble I 4 HZ 9 IRAS 04239+2436 IRAS 04248+2612 IRAS 04325+2402 IRAS 04381+2540 L1489 IRS L1527 L1551 IRS 5 L1521F-IRS LkCa 15 MWC 480 PSR B0525+21 PSR B0540+23 PSR J0348+0432 PSR J0538+2813 Teide 1 TMR-1 TMC-1A WD 0346+246 WISE 0410+1502
Hellenica World - Scientific Library
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