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139 Tauri

From Wikipedia, the free encyclopedia
Star in the constellation Taurus
139 Tauri
Observation data
Epoch J2000      Equinox J2000
ConstellationTaurus
Right ascension05h 57m 59.65632s[1]
Declination+25° 57′ 14.0799″[1]
Apparent magnitude (V)4.81[2]
Characteristics
Spectral typeB1 Ib[3][4] or B0.5 II[5]
B−Vcolor index−0.088±0.003[2]
Astrometry
Radial velocity (Rv)+8.0±4.2[6] km/s
Proper motion (μ)RA: −2.06[1]mas/yr
Dec.: −1.95[1]mas/yr
Parallax (π)2.10±0.19 mas[1]
Distance1,600 ± 100 ly
(480 ± 40 pc)
Absolute magnitude (MV)−4.4[7]
Details
Mass10.1±1.0[3] M
Radius20.7[8] R
Luminosity81,000[8] L
Surface gravity (log g)3.559±0.059[5] cgs
Temperature24,660±1,620[4] K
Rotational velocity (v sin i)140[9] km/s
Age22.5±2.6[3] Myr
Other designations
139 Tau,BD+25° 1052,HD 40111,HIP 28237,HR 2084,SAO 77775[10]
Database references
SIMBADdata

139 Tauri is a single,[11] blue-white huedstar in thezodiacconstellation ofTaurus. It is faintly visible to the naked eye with anapparent visual magnitude of 4.81.[2] The distance to this star, as determined from an annualparallax shift of2.10±0.19 mas,[1] is roughly 1,600 light years. Because this star is located near theecliptic, it is subject to occultations by the Moon. One such event was observed April 28, 1990.[12]

This is a massiveB-type lower-luminositysupergiant orbright giant star with astellar classification of B1 Ib[3][4] or B0.5 II,[5] respectively. It is around 22.5[3] million years old with a high rate of spin, showing aprojected rotational velocity of 140 km/s.[9] J. D. Rosendhal (1973) identified weakemission features associated with an asymmetricH-alphaabsorption line, providing evidence of mass loss.[13] The star has about 10[3] times themass of the Sun and around 20[8] times theSun's radius. It is radiating over 80,000[8] times theSun's luminosity from itsphotosphere at aneffective temperature of around 24,660 K.[4] Stars such as this with 10 or more solar masses are expected to end their life by exploding as aType II supernova.[14]

References

[edit]
  1. ^abcdefvan 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. ^abcAnderson, 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. ^abcdefTetzlaff, 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.
  4. ^abcdZorec, J.; et al. (2009), "Fundamental parameters of B supergiants from the BCD system. I. Calibration of the (λ1, D) parameters into Teff",Astronomy and Astrophysics,501 (1):297–320,arXiv:0903.5134,Bibcode:2009A&A...501..297Z,doi:10.1051/0004-6361/200811147,S2CID 14969137
  5. ^abcHuang, W.; Gies, D. R. (August 2008), "Stellar Rotation in Field and Cluster B Stars",The Astrophysical Journal,683 (2):1045–1051,arXiv:0805.2133,Bibcode:2008ApJ...683.1045H,doi:10.1086/590106,S2CID 18926523.
  6. ^De Bruijne, J. H. J.; Eilers, A.-C. (2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project",Astronomy & Astrophysics,546: A61,arXiv:1208.3048,Bibcode:2012A&A...546A..61D,doi:10.1051/0004-6361/201219219,S2CID 59451347.
  7. ^Wegner, W (2003). "The total-to-selective extinction ratio determined from near IR photometry of OB stars".Astronomische Nachrichten.324 (3):219–237.Bibcode:2003AN....324..219W.doi:10.1002/asna.200310081.
  8. ^abcdLamers, H. J. G. L. M (1981)."Mass loss from O and B stars".The Astrophysical Journal.245: 593.Bibcode:1981ApJ...245..593L.doi:10.1086/158835.
  9. ^abSimón-Díaz, S.; Herrero, A. (2014), "The IACOB project. I. Rotational velocities in northern Galactic O- and early B-type stars revisited. The impact of other sources of line-broadening",Astronomy & Astrophysics,562: A135,arXiv:1311.3360,Bibcode:2014A&A...562A.135S,doi:10.1051/0004-6361/201322758,S2CID 119278062.
  10. ^"139 Tau".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2018-03-30.
  11. ^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.
  12. ^Meyer, C.; et al. (1995), "Observations of lunar occultations at Observatoire de la Cote d'Azur",Astronomy and Astrophysics Supplement,110: 107,Bibcode:1995A&AS..110..107M.
  13. ^Rosendhal, J. D. (December 1973), "A survey of H-alpha emission in early-type high-luminosity stars",Astrophysical Journal,186: 909,Bibcode:1973ApJ...186..909R,doi:10.1086/152555.
  14. ^Reed, B. Cameron (June 28, 2005), "New Estimates of the Solar-Neighborhood Massive-Stars Birthrate and the Galactic Supernova Rate",The Astronomical Journal,130 (4):1652–1657,arXiv:astro-ph/0506708,Bibcode:2005AJ....130.1652R,doi:10.1086/444474,S2CID 119515135.
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