104 Tauri

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104 Tauri
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 05h 07m 27.00529s[1]
Declination +18° 38′ 42.1815″[1]
Apparent magnitude (V) 4.92[2]
Spectral type G4V[3]
B−V color index 0.64[3]
Radial velocity (Rv) +20.19[3] km/s
Proper motion (μ) RA: +534.73[1] mas/yr
Dec.: +17.93[1] mas/yr
Parallax (π) 64.79 ± 0.33[1] mas
Distance 50.3 ± 0.3 ly
(15.43 ± 0.08 pc)
Absolute magnitude (MV) 3.75±0.06[4]
Mass 1.00+0.03
[4] M
Radius 1.63±0.06[4] R
Surface gravity (log g) 4.06[2] cgs
Temperature 5,717[2] K
Metallicity [Fe/H] −0.22[2] dex
Rotational velocity (v sin i) 10.00[3] km/s
Age 10.15[2] Gyr
Other designations
m Tau, 104 Tau, BD+18 779, GJ 188, HD 32923, HIP 23835, HR 1656, SAO 94332.[5]

104 Tauri (104 Tau) is the Flamsteed designation for a star in the equatorial constellation of Taurus. It has an apparent magnitude of 4.92, which is bright enough to be seen with the naked eye. Based upon parallax measurements, this star is located about 50 light years from the Sun.[1]

The apparent brightness of this star indicates that it is a young, population I star. However, the chemical abundances in its outer atmosphere tell a different story, suggesting that it is an population II star with an age of 12−13 billion years. This discrepancy may indicate that the star has undergone a period of mass accretion. Possible scenarios indicate that the star has either undergone a merger with a close companion, or else interacted with the progenitor cloud of the nearby open cluster NGC 2516.[6]

The star displays convincing evidence for an infrared excess, suggesting the presence of a circumstellar debris disk of dust.[7]


  1. ^ a b c d e f van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752free to read, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d e Ramírez, I.; et al. (February 2013), "Oxygen abundances in nearby FGK stars and the galactic chemical evolution of the local disk and halo", The Astrophysical Journal, 764 (1): 78, arXiv:1301.1582free to read, Bibcode:2013ApJ...764...78R, doi:10.1088/0004-637X/764/1/78. 
  3. ^ a b c d White, Russel J.; et al. (June 2007), "High-Dispersion Optical Spectra of Nearby Stars Younger Than the Sun", The Astronomical Journal, 133 (6): 2524–2536, arXiv:0706.0542free to read, Bibcode:2007AJ....133.2524W, doi:10.1086/514336. 
  4. ^ a b c Bernkopf, Jan; Fuhrmann, Klaus (June 2006), "Local subgiants and time-scales of disc formation", Monthly Notices of the Royal Astronomical Society, 369 (2): 673−676, Bibcode:2006MNRAS.369..673B, doi:10.1111/j.1365-2966.2006.10326.x. 
  5. ^ "m Tau -- Double or multiple star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2013-08-12. 
  6. ^ Fuhrmann, K.; et al. (December 2012), "Archeology of an Ancient Star", The Astrophysical Journal, 761 (2): 8, Bibcode:2012ApJ...761..159F, doi:10.1088/0004-637X/761/2/159, 159. 
  7. ^ Holmes, E. K.; et al. (June 2003), "A Survey of Nearby Main-Sequence Stars for Submillimeter Emission", The Astronomical Journal, 125 (6): 3334−3343, Bibcode:2003AJ....125.3334H, doi:10.1086/375202.