Epoch J2000.0 Equinox J2000.0
|Right ascension||04h 35m 55.23907s|
|Declination||+16° 30′ 33.4885″|
|Apparent magnitude (V)||0.75–0.95|
|Evolutionary stage||Red giant branch|
|Spectral type||K5+ III|
|Apparent magnitude (J)||−2.095|
|U−B color index||+1.92|
|B−V color index||+1.44|
|Radial velocity (Rv)||+54.26±0.03 km/s|
|Proper motion (μ)||RA: 63.45±0.84 mas/yr |
Dec.: −188.94±0.65 mas/yr
|Parallax (π)||49.97 ± 0.75 mas|
|Distance||65.3 ± 1.0 ly |
(20.0 ± 0.3 pc)
|Absolute magnitude (MV)||−0.641±0.034|
|Surface gravity (log g)||1.45±0.3 cgs|
|Metallicity [Fe/H]||−0.33±0.1 dex|
|Rotational velocity (v sin i)||3.5±1.5 km/s|
Aldebaran // , designated α Tauri (Latinized to Alpha Tauri, abbreviated Alpha Tau, α Tau), is an orange 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 red giant, 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.
The traditional name Aldebaran derives from the Arabic al Dabarān, meaning "the follower", because it seems to follow the Pleiades.In 2016, the International Astronomical Union Working Group on Star Names (WGSN) approved the proper name Aldebaran for this star.
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.
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.
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.
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.
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.A series of 49 occultations occurred starting on 29 January 2015 and ending at 3 September 2018. Each event was visible from points in the northern hemisphere or close to the equator; people in e.g. Australia or South Africa can never observe an Aldebaran occultation since it is too far south of the ecliptic. A reasonably accurate estimate for the diameter of Aldebaran was obtained during the occultation of 22 September 1978. Aldebaran is in conjunction with the Sun around June 1 of each year.
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.
On 11 March AD 509, a lunar occultation of Aldebaran was observed in Athens, Greece. 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. Due to precession of the equinoxes, 5,000 years ago the equinox (Northern Hemisphere)|vernal equinox was close to Aldebaran.
English astronomer William Herschel discovered a faint companion to Aldebaran in 1782;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.
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.
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.
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.It had previously been used to calibrate instruments on board the Hubble Space Telescope.
Aldebaran is listed as the spectral standard for type K5+ III stars.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).
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. Asteroseismology has determined that it is about 16% more massive than the Sun, 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 . It is 44 times the diameter of the Sun, approximately 61 million kilometres.
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.Modern studies show a smaller amplitude, with some showing almost no variation. Hipparcos photometry shows an amplitude of only about 0.02 magnitudes and a possible period around 18 days. Intensive ground-based photometry showed variations of up to 0.03 magnitudes and a possible period around 91 days. 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.
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. Gauss. Any resulting soft X-ray emissions from this region may be attenuated by the chromosphere, although ultraviolet emission has been detected in the spectrum. 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. This stellar wind may be generated by the weak magnetic fields in the lower atmosphere.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
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. 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.
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.
|α Tau|| Apparent|
Some surveys, for example Gaia Data Release 2,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. A spectral type of M2.5 has been published for Alpha Tauri B.
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.
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.
In 2015 a study showed stable long-term evidence for both a planetary companion and stellar activity. 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. This would place it and any of its moons in the habitable zone.An asteroseismic analysis of the residuals to the planet fit has determined that Aldebaran
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.It is assumed that what it was following is the Pleiades. A variety of transliterated spellings have been used, with the current Aldebaran becoming standard relatively recently.
This easily seen and striking star in its suggestive asterism is a popular subject for ancient and modern myths.
The name Aldebaran or Alpha Tauri has been adopted many times, including
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,often linked to Nazi UFOs. 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.
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.
Alpha Cancri, also named Acubens, is a star system in the constellation of Cancer.
Theta Tauri is a wide double star in the constellation of Taurus and a member of the Hyades open cluster.
Gamma Tauri is either a solitary, binary or double star that marks the tip of the "V" in the constellation of Taurus. It is a member of, and located within about 2.5 parsecs of the center of, the Hyades star cluster, the nearest open cluster to the Sun. Based upon parallax measurements, Gamma Tauri is approximately 154 light-years from the Sun.
Upsilon Tauri is a solitary, white-hued star in the zodiac constellation of Taurus, and is a member of the Hyades star cluster. It is faintly visible to the naked eye with an apparent visual magnitude of +4.28. Based upon an annual parallax shift of 21.21 mas seen from Earth, it is around 154 light years from the Sun.
Rho Tauri is a star in the constellation Taurus and a member of the Hyades star cluster.
Sigma Tauri is the Bayer designation for a pair of white-hued stars in the zodiac constellation of Taurus. The system is a visual double star, whose components are designated σ1 Tauri and σ2 Tauri, with the latter being the more northerly star. The two are separated by 7.2 arcminutes on the sky and can be readily split with a pair of binoculars. They have apparent visual magnitudes of +5.07 and +4.70, respectively, which indicated they are both visible to the naked eye. Based upon parallax measurements, σ1 Tauri is about 147 light years from the Sun, while σ2 Tauri is 156 light years distant.
22 Tauri is a component of the Asterope double star in the Pleiades open cluster. 22 Tauri is the stars' Flamsteed designation. It is situated near the ecliptic and thus is subject to lunar occultation. The star has an apparent visual magnitude of 6.43, which is near the lower threshold of visibility to the naked eye. Anybody attempting to view the object is likely to instead see the Asterope pair as a single elongated form of magnitude 5.6. Based upon an annual parallax shift of 7.35 mas, this star is located 444 light years away from the Sun. It is moving further from the Earth with a heliocentric radial velocity of +7 km/s.
Delta¹ Tauri is a double star in the zodiac constellation of Taurus. Based upon an annual parallax shift of 20.96 mas as seen from Earth, it is located roughly 156 light-years distant from the Sun. The system is faintly visible to the naked eye with a combined apparent visual magnitude of +3.772. It is considered a member of the Hyades cluster.
Delta2 Tauri is a solitary, white-hued star in the zodiac constellation of Taurus. Based upon an annual parallax shift of 20.21 mas as seen from Earth, it is located roughly 161 light years distant from the Sun. It is separated from δ1 Tauri by 0.3° on the sky and is faintly visible to the naked eye with an apparent visual magnitude of +4.80. The star is considered a member of the Hyades cluster.
21 Aquilae is a solitary variable star in the equatorial constellation of Aquila. It has the variable star designation V1288 Aql; 21 Aquilae is its Flamsteed designation. This object is visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of 5.14. The star is located at a distance of around 740 light-years from Earth, give or take a 30 light-year margin of error. It is moving closer to the Earth with a heliocentric radial velocity of –5 km/s.
41 Aurigae is a binary star system located around 310–316 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a dim, white-hued star with a combined apparent visual magnitude of 5.83. This system is moving further from the Earth with a heliocentric radial velocity of 31 km/s. It is a probable member of the Hyades Supercluster.
3 Cancri is a single star in the zodiac constellation of Cancer, located around 810 light years from the Sun. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.60. This object is moving further from the Earth with a heliocentric radial velocity of +39.5 km/s, and may be a member of the Hyades group. It is located near the ecliptic and thus is subject to lunar eclipses.
20 Canum Venaticorum is a single variable star in the northern constellation of Canes Venatici, located 238 light years from the Sun. This object has the variable star designation AO Canum Venaticorum; 20 Canum Venaticorum is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star with a baseline apparent visual magnitude of +4.72. The star is moving further from the Earth with a heliocentric radial velocity of +9 km/s. Eggen (1971) listed this star as a member of the Hyades Stream.
119 Tauri is a red supergiant star in the constellation Taurus. It is a semiregular variable and its angular diameter has been measured at about 10 mas.
C3 Centauri is a suspected astrometric binary star system in the southern constellation of Centaurus. It has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.46. The distance to this object is approximately 342 light years based on parallax. It is a member of the Hyades Stream of co-moving stars.
2 Ursae Minoris is a single star a few degrees away from the northern celestial pole. Despite its Flamsteed designation, the star is actually located in the constellation Cepheus. This changed occurred when the constellation boundaries were formally set in 1930 by Eugene Delporte. Therefore, the star is usually referred only by its catalog numbers such as HR 285 or HD 5848. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.244. This object is located 280 light years away and is moving further from the Earth with a heliocentric radial velocity of +8 km/s. It is a candidate member of the Hyades Supercluster.
21 Camelopardalis is a star in the northern circumpolar constellation of Camelopardalis, located around 650 light years away from the Sun. It is a challenge to view with the naked eye even under excellent viewing conditions, having an apparent visual magnitude of 6.9. This is one of the fainter stars with a Flamsteed designation, one of only 220 below the magnitude cutoff for the Bright Star Catalogue. It is moving closer to the Earth with a heliocentric radial velocity of −15.5 km/s.
Pi Leonis, Latinized from π Leonis, is a single star in the zodiac constellation Leo. It is a red hued star that is visible to the naked eye with an apparent visual magnitude of 4.70. This object is located at a distance of some 410 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +22 km/s. Because the star lies near the ecliptic it is subject to occultations by the Moon.
90 Tauri is a star in the zodiac constellation of Taurus, located 144 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.27. 90 Tauri is a member of the Hyades cluster and is listed as a double star.
139 Tauri is a single, blue-white hued star in the zodiac constellation of Taurus. It is faintly visible to the naked eye with an apparent visual magnitude of 4.81. The distance to this star, as determined from an annual parallax shift of 2.10±0.19 mas, is roughly 1,600 light years. Because this star is located near the ecliptic, it is subject to occultations by the Moon. One such event was observed April 28, 1990.
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