Astronomy:10 Tauri

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Short description: Star in the constellation Taurus
10 Tauri
Chart showing the position of the stars in the constellation Taurus
Location of 10 Tauri (circled)
Observation data
Equinox J2000.0]] (ICRS)
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[1] mas
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. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Cowley, A. P. et al. (December 1967), "Spectral classification and photometry of high proper motion stars", Astronomical Journal 72: 1334−1340, doi:10.1086/110413, Bibcode: 1967AJ.....72.1334C. 
  3. ↑ 3.0 3.1 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. doi:10.1086/191373. Bibcode: 1989ApJS...71..245K. 
  4. ↑ 4.0 4.1 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, doi:10.1051/0004-6361:20035959, Bibcode: 2004A&A...418..989N. 
  5. ↑ 5.0 5.1 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. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 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, doi:10.1088/0004-637X/746/1/101, Bibcode: 2012ApJ...746..101B . See Table 10.
  7. ↑ 7.0 7.1 7.2 7.3 Soubiran, C.; Creevey, O. L.; Lagarde, N.; Brouillet, N.; Jofré, P.; Casamiquela, L.; Heiter, U.; Aguilera-Gómez, C. et al. (2024-02-01). "Gaia FGK benchmark stars: Fundamental Teff and log g of the third version". Astronomy and Astrophysics 682: A145. doi:10.1051/0004-6361/202347136. ISSN 0004-6361. Bibcode: 2024A&A...682A.145S.  10 Tauri's database entry at VizieR.
  8. ↑ 8.0 8.1 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, doi:10.1051/0004-6361/201014948, Bibcode: 2010A&A...521A..12M 
  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, doi:10.1093/mnras/stv483, Bibcode: 2015MNRAS.449.3160R. 
  10. ↑ van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL.  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. doi:10.1111/j.1365-2966.2005.09848.x. Bibcode: 2006MNRAS.366..283G. 
  12. ↑ Ian Ridpath's Star Tales - Psalterium Georgii



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