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Aldebaran

Coordinates: Sky map 04h 35m 55.2s, +16° 30′ 33″
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For other uses, see Aldebaran (disambiguation).
Not to be confused with Alderaan or Alderaan (astronomy).
Aldebaran

The position of Aldebaran in the Taurus constellation.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Taurus
Right ascension 04h 35m 55.239s[1]
Declination +16° 30′ 33.49″[1]
Apparent magnitude (V) 0.75-0.95[2]
Characteristics
Spectral type K5III[1]
Apparent magnitude (J) -2.10[1]
U−B color index 1.90
B−V color index 1.54
Variable type LB[2]
Astrometry
Radial velocity (Rv)+54.26 ±0.03[1] km/s
Proper motion (μ) RA: 62.78 ±0.89[1] mas/yr
Dec.: −189.35 ±0.58[1] mas/yr
Parallax (π)50.09 ± 0.95 mas
Distance65 ± 1 ly
(20.0 ± 0.4 pc)
Absolute magnitude (MV)−0.63
Details
Mass1.7[3] M☉
Radius44.2 ± 0.9[4] R☉
Luminosity518 ± 32[5] L☉
Surface gravity (log g)1.59[5] cgs
Temperature3,910[5] K
Metallicity70% Sun[3]
Metallicity [Fe/H]–0.34[5] dex
Rotation643 days[6]
Other designations
87 Tauri, Alpha Tauri, BD +16°629, GJ 171.1, GJ 9159, HD 29139, HIP 21421, HR 1457, SAO 94027
Database references
SIMBADdata
ARICNSdata

Aldebaran /ælˈdɛbərən/[7][8] (α Tau, α Tauri, Alpha Tauri) is an orange giant star located about 65 light years away in the zodiac constellation of Taurus. With an average apparent magnitude of 0.87 it is the brightest star in the constellation and is one of the brightest stars in the nighttime sky. The name Aldebaran is Arabic (الدبران al-dabarān) and translates literally as "the follower", presumably because this bright star appears to follow the Pleiades, or "Seven Sisters" star cluster in the night sky.[3] It's one of the brightest stars in the night sky.

In 1997 a substellar companion was reported but subsequent observations have not confirmed this claim.

Physical properties

Size comparison between Aldebaran and the Sun.

Aldebaran is classified as a type K5III star. It is an orange giant star that has moved off the main sequence line of the Hertzsprung–Russell diagram. It has exhausted the hydrogen fuel in its core leading to core compression from gravity and helium fusion ignition through the triple-alpha fusion process.[9] Hydrogen fusion is now occurring in a shell around the helium core. The helium flash ignition expanded the star to a diameter of 44.2 times the diameter of the Sun,[4][10] approximately 61 million kilometres (see 10 gigametres for similar sizes). The Hipparcos satellite has measured it as 65.1 light years (20.0 pc) away, and it shines with 425 times the Sun's luminosity.[3]

Aldebaran is a slightly variable star, of the slow irregular variable type LB. It varies by about 0.2 in apparent magnitude from 0.75 to 0.95.[2] With a near-infrared J band magnitude of −2.1,[1] only Betelgeuse (−2.9), R Doradus (−2.6), and Arcturus (−2.2) are brighter.

Visibility

Aldebaran is one of the easiest stars to find in the night sky, partly due to its brightness and partly due to its spatial relation to one of the more noticeable asterisms in the sky. 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 Hyades open 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 150 light years.

In this predawn occultation, Aldebaran has just reappeared on the dark limb of the waning crescent Moon (July 1997 still frame captured from video).

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. This event will next occur on October 29, 2015, then again on December 23, 2015. A reasonably accurate estimate for the diameter of Aldebaran was obtained during the September 22, 1978 occultation.[11] Aldebaran is in conjunction with the Sun around June 1 of each year.[12]

Double star

Five faint stars appear close enough to Aldebaran in its visual field for astronomers to consider it a double star association. These 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. The better known characteristics of these optical double stars are listed in the table below with the primary star, Aldebaran (Alpha Tauri A), shown for reference.[13]

Star
α Tauri 		Right
ascension 		Declination Apparent
magnitude 		Distance
(light years) 		Proper motion
(mas/yr) 		Spectral
type 		Absolute
magnitude 		Other names References
A 04h 35m 55.239s +16° 30′ 33.49″ 0.85 65 RA: 62.78 ±0.89
Dec.: −189.35 ±0.58		 K5III −0.63 Aldebaran,
GJ 171.1 A,
ADS 3321 A,
BD +16°629A		 [1]
B 04h 35m 57.0s +16° 30′ 22″ 13.6 RA: 64 ±25
Dec.: -191 ±25		 M2V 11.98 GJ 171.1 B [14]
C 04h 35m 55.5s +16° 30′ 38″ 9.4 ADS 3321 C [15][16]
D 04h 35m 55.5s +16° 30′ 38″ 11.8 ADS 3321 D [15][17]
E 04h 35m 53.8s +16° 31′ 08″ BD +16°629E [18]
F 04h 33.3m +16° 22′ 13.6 BD +16°629F [19]

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.[20]

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.[15]

Claims of a planetary system

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.[21] Subsequent observations have not confirmed any substellar companions in orbit around Aldebaran.[22]

Etymology

From Arabic الدبران (al-dabarān), meaning "the follower" (of the Pleiades)

Names in other languages

In Persia it was known as Tascheter.

The Romans called it Palilicium.

In the Middle Ages it was sometimes called Cor Tauri (the Heart of the Bull/Taurus).

In Chinese it is known as 畢宿五 (Bìxiùwŭ, the Fifth Star of the Net).

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).

Myths

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 is providing 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".[23]
  • 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.[24]
  • In Hindu mythology Aldebaran is known by the name Rohini and is the fourth of the 27 daughters of Daksha given to God Chandra(moon) as wives. The Moon God enamoured by the beauty of Rohini started spending all his time with her neglecting the others. (This amounts to moon not going round the constellations of zodiac and remaining in one place!). Daksha got angry and cursed him to suffer by slow dessication. After pleading to the lord Shiva the curse was held at bay and the moon was rejuvenated by shiva's grace for 15 days and dessicated for another 15 days thus waning and waxing to make a lunar month.

See also

References

  1. ^ a b c d e f g h i "V* alf Tau -- Variable Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-16.
  2. ^ a b c "Query= alf Tau". General Catalogue of Variable Stars. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-16.
  3. ^ a b c d James B. Kaler (May 22, 2009). "Aldebaran". Stars. Archived from the original on 10 January 2010. Retrieved 2009-12-20. {{cite web}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help)
  4. ^ a b Richichi, A.; Roccatagliata, V. (2005). "Aldebaran's angular diameter: How well do we know it?". Astronomy & Astrophysics. 433 (1): 305–312. arXiv:astro-ph/0502181. Bibcode:2005A&A...433..305R. doi:10.1051/0004-6361:20041765. We derive an average value of 19.96±0.03 milliarcsec for the uniform disk diameter. The corresponding limb-darkened value is 20.58±0.03 milliarcsec, or 44.2±0.9 R☉.
  5. ^ a b c d Piau, L.; et al. (February 2011), "Surface convection and red-giant radius measurements", Astronomy and Astrophysics, 526: A100, arXiv:1010.3649, Bibcode:2011A&A...526A.100P, doi:10.1051/0004-6361/201014442
  6. ^ Koncewicz, R.; Jordan, C. (January 2007), "OI line emission in cool stars: calculations using partial redistribution", Monthly Notices of the Royal Astronomical Society, 374 (1): 220–231, Bibcode:2007MNRAS.374..220K, doi:10.1111/j.1365-2966.2006.11130.x{{citation}}: CS1 maint: unflagged free DOI (link)
  7. ^ Oxford Dictionary: Aldebaran
  8. ^ Merriam-Webster: Aldebaran
  9. ^ http://iopscience.iop.org/0004-637X/618/1/493/fulltext/59619.text.html
  10. ^ Richichi & Roccatagliata (2005) derived an angular diameter of 20.58±0.03 milliarcsec, which given a distance of 65 light years yields a diameter of 61 million km.
  11. ^ White, N. M. (June 1979). "Lunar occultation of the Hyades and diameters of Alpha Tauri and Theta-1 Tauri". The Astronomical Journal. 84: 872–876. Bibcode:1979AJ.....84..872W. doi:10.1086/112489.
  12. ^ Star Maps created using XEphem (2008). "LASCO Star Maps (identify objects in the field of view for any day of the year)". Large Angle and Spectrometric Coronagraph Experiment (LASCO). Retrieved 2012-06-01. 2012 (with Venus and Mercury) and 2011
  13. ^ "VizieR Detailed Page CCDM===04359+1631". VizieR. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-30.
  14. ^ "GJ 171.1 B -- Star in double system". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-30.
  15. ^ a b c Griffin, R. F. (September 1985). "Alpha Tauri CD - A well-known Hyades binary". Astronomical Society of the Pacific, Publications (ISSN 0004-6280). 97: 858–859. Bibcode:1985PASP...97..858G. doi:10.1086/131616.
  16. ^ "ADS 3321 C -- Star in double system". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-30.
  17. ^ "ADS 3321 D -- Star in double system". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-30.
  18. ^ "BD+16 629E -- Star in double system". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-30.
  19. ^ "BD+16 629F -- Star in double system". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-30.
  20. ^ Poveda, A.; Herrera, M. A.; Allen, C.; Cordero, G.; Lavalley, C. (April 1994). "Statistical studies of visual double and multiple stars. II. A catalogue of nearby wide binary and multiple systems". Revista Mexicana de Astronomia y Astrofisica. 28 (1): 43–89. Bibcode:1994RMxAA..28...43P.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  21. ^ Hatzes, A., Cochran, W. (1993). "Long-period radial velocity variations in three K giants". The Astrophysical Journal. 413 (1): 339–348. Bibcode:1993ApJ...413..339H. doi:10.1086/173002.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  22. ^ Hatzes, A., Cochran, W. (1998). "On the nature of the radial velocity variability of Aldebaran - A search for spectral line bisector variations". Monthly Notices of the Royal Astronomical Society. 293 (4): 469–478. arXiv:astro-ph/9712312. Bibcode:1998MNRAS.293..469H. doi:10.1046/j.1365-8711.1998.01186.x.{{cite journal}}: CS1 maint: multiple names: authors list (link) CS1 maint: unflagged free DOI (link)
  23. ^ Moser, Mary B.; Stephen A. Marlett (2005). Comcáac quih yaza quih hant ihíip hac: Diccionario seri-español-inglés (PDF) (in Spanish and English). Hermosillo, Sonora and Mexico City: Universidad de Sonora and Plaza y Valdés Editores.{{cite book}}: CS1 maint: unrecognized language (link)
  24. ^ p. 30, Aboriginal People and Their Plants, Philip A. Clarke, New South Wales, Rosenberg Publishing Pty Ltd, 2007.

Media related to Aldebaran at Wikimedia Commons


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