10 Tauri

10 Tauri
Chart showing the position of the stars in the constellation Taurus
Location of 10 Tauri (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 03h 36m 52.38s[1]
Declination +00° 24′ 06.0″[1]
Apparent magnitude (V) 4.29[2]
Characteristics
Evolutionary stage subgiant[1]
Spectral type F9IV-V[3]
U−B color index +0.08[2]
B−V color index +0.58[2]
Astrometry
Radial velocity (Rv)+27.8±0.5[4] km/s
Proper motion (μ) RA: −232.563[1] mas/yr
Dec.: −481.472[1] mas/yr
Parallax (π)71.8370±0.01503 mas[1]
Distance45.402 ± 0.009 ly
(13.920 ± 0.003 pc)
Absolute magnitude (MV)+3.60[5]
Details
Mass1.139±0.016[6] M☉
Radius1.622±0.024[6] R☉
Luminosity3.042±0.042[6] L☉
Surface gravity (log g)4.06±0.03[7] cgs
Temperature6,000±59[7] K
Metallicity [Fe/H]−0.08±0.01[7] dex
Rotation17.6 days[8]
Rotational velocity (v sin i)2.4[5] km/s
Age5.7±0.4[6] Gyr
Other designations
10 Tau, BD−00°572, FK5 1101, GJ 147, HD 22484, HIP 16852, HR 1101, SAO 111292, LHS 1569, LTT 11194
Database references
SIMBADdata

10 Tauri is a single[9] star in the zodiac constellation of Taurus. It can be seen with the naked eye, having an apparent visual magnitude of 4.29.[2] An annual parallax shift of 71.62[10] mas provides a distance estimate of 45.5 light years. It is moving further from the Sun with a radial velocity of +28 km/s[4] and has a relatively high proper motion.[2]

The star has a stellar classification of F9IV-V,[3] indicating that it is an F-type star between main sequence and subgiant. Modles indicate that it is a subgiant,[1] having exhausted its core hydrogen and evolved away from the main sequence. It is around 5.7[6] billion years old with a rotation period of 17.6 days.[8] The star has 1.14 times the mass of the Sun and 1.6 times the Sun's radius. It is radiating three[6] times the Sun's luminosity from its photosphere at an effective temperature of 6,000 K.[7]

A debris disk has been identified orbiting 10 Tauri, based on excess infrared radiation detected by IRAS/ISO.[11]

10 Tauri was the brightest star in the obsolete constellation Psalterium Georgii (Harpa Georgii).[12]

References

  1. ^ a b c d e f g Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c d e Cowley, A. P.; et al. (December 1967), "Spectral classification and photometry of high proper motion stars", Astronomical Journal, 72: 1334−1340, Bibcode:1967AJ.....72.1334C, doi:10.1086/110413.
  3. ^ a b Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins Catalog of Revised MK Types for the Cooler Stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  4. ^ a b Nordström, B.; et al. (May 2014), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ~14000 F and G dwarfs", Astronomy and Astrophysics, 418: 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959, S2CID 11027621.
  5. ^ a b Pizzolato, N.; Maggio, A.; Sciortino, S. (September 2000), "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases", Astronomy and Astrophysics, 361: 614–628, Bibcode:2000A&A...361..614P
  6. ^ a b c d e f Boyajian, Tabetha S.; et al. (February 2012), "Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars", The Astrophysical Journal, 746 (1): 101, arXiv:1112.3316, Bibcode:2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101, S2CID 18993744. See Table 10.
  7. ^ a b c d Soubiran, C.; Creevey, O. L.; Lagarde, N.; Brouillet, N.; Jofré, P.; Casamiquela, L.; Heiter, U.; Aguilera-Gómez, C.; Vitali, S.; Worley, C.; de Brito Silva, D. (2024-02-01). "Gaia FGK benchmark stars: Fundamental Teff and log g of the third version". Astronomy and Astrophysics. 682: A145. arXiv:2310.11302. Bibcode:2024A&A...682A.145S. doi:10.1051/0004-6361/202347136. ISSN 0004-6361. 10 Tauri's database entry at VizieR.
  8. ^ a b Maldonado, J.; et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics, 521: A12, arXiv:1007.1132, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948, S2CID 119209183
  9. ^ Rodriguez, David R.; et al. (May 2015), "Stellar multiplicity and debris discs: an unbiased sample", Monthly Notices of the Royal Astronomical Society, 449 (3): 3160–3170, arXiv:1503.01320, Bibcode:2015MNRAS.449.3160R, doi:10.1093/mnras/stv483.
  10. ^ van Leeuwen, F. (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. Vizier catalog entry
  11. ^ J.S. Greaves; D.A. Fischer; M.C. Wyatt (2006). "Metallicity, Debris Discs and Planets". Monthly Notices of the Royal Astronomical Society. 366 (1): 283–286. Bibcode:2006MNRAS.366..283G. doi:10.1111/j.1365-2966.2005.09848.x.
  12. ^ Ian Ridpath's Star Tales - Psalterium Georgii
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