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]
Characteristics
Spectral type G4V [3]
B−V color index 0.64 [3]
Astrometry
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  mas [1]
Distance 50.3 ± 0.3  ly
(15.43 ± 0.08  pc)
Absolute magnitude  (MV)3.75±0.06 [4]
Details
Mass 1.00+0.03
−0.04 [4]   M☉
Radius 1.63±0.06 [4]   R☉
Luminosity 2.41 [5]   L☉
Habitable zone inner limit1.17 [6] AU
Habitable zone outer limit2.76 [6] AU
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 [7]
Database references
SIMBAD data

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] It is moving further from the Sun with a heliocentric radial velocity of +20 km/s. [3]

This star has a stellar classification of G4 V, [3] which suggests it is an ordinary G-type main-sequence star that is generating energy through hydrogen fusion at its stellar core. It is an estimated 10 [2]  billion years old and is spinning with a projected rotational velocity of 10 km/s. [3] The star has about the same mass as the Sun, with 1.6 times the Sun's radius. [4] It is radiating 2.4 [5] times the Sun's luminosity from its photosphere at an effective temperature of 5,717  K . [2]

104 Tauri appears to have a modest barium enrichment compared to iron. This may indicate that the star had accreted stellar wind of a companion star in the asymptotic giant branch, which has since evolved into a white dwarf. [8]

The star displays convincing evidence for an infrared excess, suggesting the presence of a circumstellar debris disk of dust. [9] It also presents a statistically significant difference on proper motion measurements taken by the Hipparcos and Gaia spacecrafts, suggesting the presence of an orbiting exoplanet. [6]

On 24 July 2028, it will be occulted by Venus over Japan, East Siberia and the Pacific Ocean. [10] : 165 

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752 , Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID   18759600.
  2. 1 2 3 4 5 6 7 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: 1301.1582 , Bibcode:2013ApJ...764...78R, doi:10.1088/0004-637X/764/1/78, S2CID   118751608.
  3. 1 2 3 4 5 6 7 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: 0706.0542 , Bibcode:2007AJ....133.2524W, doi:10.1086/514336, S2CID   122854.
  4. 1 2 3 4 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. 1 2 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
  6. 1 2 3 Painter, Katie E.; Bowler, Brendan P.; Franson, Kyle; Becker, Juliette C.; Burt, Jennifer A. (2025-06-26), "Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory", The Astronomical Journal, arXiv: 2506.21768 .
  7. ↑ "m Tau -- Double or multiple star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg , retrieved 2013-08-12.
  8. ↑ Fuhrmann, K.; Chini, R.; Kaderhandt, L.; Chen, Z.; Lachaume, R. (2017-07-21). "The barium-to-iron enrichment versus age relation of ancient disc stars". Monthly Notices of the Royal Astronomical Society. 471 (3). Oxford University Press (OUP): 3768–3774. Bibcode:2017MNRAS.471.3768F. doi: 10.1093/mnras/stx1848 . ISSN   0035-8711.
  9. ↑ 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 .
  10. ↑ Meeus, Jan (2002). "Mutual occultations of planets". More Mathematical Astronomy Morsels (PDF). pp. 174–185. ISBN   0943396743.


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