114 Tauri

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This article is about o Tauri. It is not to be confused with ο (Omicron) Tauri.
114 Tauri
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 05h 27m 38.08406s[1]
Declination +21° 56′ 13.0738″[1]
Apparent magnitude (V) 4.88[2]
Characteristics
Spectral type B2.5 IV[3] or B2.5 V[4]
B−V color index −0.14[2]
Astrometry
Radial velocity (Rv)16.5±0.1[2] km/s
Proper motion (μ) RA: +0.05[1] mas/yr
Dec.: −7.06[1] mas/yr
Parallax (π)5.22 ± 0.21[1] mas
Distance620 ± 30 ly
(192 ± 8 pc)
Absolute magnitude (MV)−1.58[5]
Details[6]
Mass7.3±0.3 M☉
Radius3.9±0.4 R☉
Luminosity2,454+497
−365 L☉
Surface gravity (log g)4.15±0.07 cgs
Temperature20,700±200 K
Rotational velocity (v sin i)10[7] km/s
Age22.0±3.1[8] Myr
Other designations
o Tau, 114 Tau, BD+21° 847, HD 35708, HIP 25539, HR 1810, SAO 77184, WDS J05276+2156A[9]
Database references
SIMBADdata

114 Tauri, or o Tauri, is a single,[10] blue-white hued star in the zodiac constellation of Taurus. It is a faint star but visible to the naked eye with an apparent visual magnitude of 4.88.[2] The distance to this star, as determined from its annual parallax shift of 5.22±0.21 mas,[1] is roughly 620 light years. It is moving further from the Sun with a heliocentric radial velocity of 16.5 km/s, having come as close as 240 ly (75 pc) some 9.6 million years ago.[2] It is a member of the Cas-Tau OB association of co-moving stars,[6] and has a peculiar velocity of 8.3 km/s.[11]

Grenier et al. (1999) assigned this star to a stellar classification of B2.5 IV,[3] which matches the luminosity class of an evolving subgiant star. Abt (2008) listed it as a B-type main-sequence star with a class of B2.5 V.[4] With an age of about 22[8] million years, 114 Tauri has an estimated 7 times the mass of the Sun and four times the Sun's radius. The star is radiating about 2,454 times the Sun's luminosity from its photosphere at an effective temperature of around 20,700 K.[6] It appears to be have a relatively low rotation rate for a star of its mass and age, showing a projected rotational velocity of 10 km/s.[7]

References[]

  1. ^ a b c d e f 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.
  2. ^ a b c d e 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.
  3. ^ a b Grenier, S.; et al. (1999), "Radial velocities. Measurements of 2800 B2-F5 stars for HIPPARCOS" (PDF), Astronomy and Astrophysics Supplement, 137 (3): 451, Bibcode:1999A&AS..137..451G, doi:10.1051/aas:1999489
  4. ^ a b Abt, Helmut A. (2008), "Visual Multiples. IX. MK Spectral Types", The Astrophysical Journal Supplement Series, 176 (1): 216–217, Bibcode:2008ApJS..176..216A, doi:10.1086/525529
  5. ^ Huang, W.; et al. (2012), "A catalogue of Paschen-line profiles in standard stars", Astronomy & Astrophysics, 547: A62, arXiv:1210.7893, Bibcode:2012A&A...547A..62H, doi:10.1051/0004-6361/201219804, S2CID 119286159.
  6. ^ a b c Nieva, María-Fernanda; Przybilla, Norbert (2014), "Fundamental properties of nearby single early B-type stars", Astronomy & Astrophysics, 566: A7, arXiv:1412.1418, Bibcode:2014A&A...566A...7N, doi:10.1051/0004-6361/201423373, S2CID 119227033.
  7. ^ a b Strom, Stephen E.; et al. (2005), "B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?", The Astronomical Journal, 129 (2): 809–828, arXiv:astro-ph/0410337, Bibcode:2005AJ....129..809S, doi:10.1086/426748, S2CID 15059129.
  8. ^ a b Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
  9. ^ "o Tau". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-03-25.
  10. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  11. ^ Bobylev, V. V.; Bajkova, A. T. (August 2013), "Galactic kinematics from a sample of young massive stars", Astronomy Letters, 39 (8): 532–549, arXiv:1307.1677, Bibcode:2013AstL...39..532B, doi:10.1134/S106377371308001X, S2CID 118568203.

External links[]

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