32 Tauri
  | |
| Observation data EpochJ2000.0EquinoxJ2000.0 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 03h56m52.077s[1] |
| Declination | +22° 28′ 40.70″[1] |
| Apparent magnitude(V) | 5.62[2] |
| Characteristics | |
| Spectral type | F2IVs[3] |
| U−Bcolor index | +0.00[4] |
| B−Vcolor index | +0.345±0.004[2] |
| Astrometry | |
| Radial velocity(Rv) | +31.90[5]km/s |
| Proper motion(μ) | RA:+70.674mas/yr[1] Dec.:−114.026mas/yr[1] |
| Parallax(π) | 22.5957 ± 0.0385mas[1] |
| Distance | 144.3 ± 0.2ly (44.26 ± 0.08pc) |
| Absolute magnitude(MV) | 2.42[6] |
| Details | |
| Mass | 2.04[7]M☉ |
| Radius | 2.75[7]R☉ |
| Luminosity | 15.4[7]L☉ |
| Surface gravity(logg) | 3.87[7]cgs |
| Temperature | 6.901[7]K |
| Metallicity[Fe/H] | −0.19[8]dex |
| Rotational velocity(vsini) | 19.7[9]km/s |
| Age | 2.1[10]Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
32 Tauriis theFlamsteed designationfor a solitary[12]starin thezodiacconstellationofTaurus.It has avisual magnitudeof 5.64,[4]making it visible to the naked eye from suburban skies (according to theBortle scale). The position of this star near theecliptic planemeans that it is subject tooccultationsby theMoon.[13]Parallaxmeasurements put it at a distance of 144light yearsfrom theSun.[1]It is drifting further away with aradial velocityof +31.9[5]km/s, having come to within 88.9 light-years some 759,000 years ago.[2]
Thespectrumof this star matches astellar classificationof F2IVs,[3]with theluminosity classof IV indicating that this star has reached thesubgiantstage and is in the process of evolving into agiant star.It has twice the mass of the sun with nearly three times theSun's radius,but 15 times the Sun's luminosity[7]and about half the Sun's age.[10]The abundance of elements other than hydrogen and helium is lower in this star than in the Sun.[10]Theeffective temperatureof the star'souter atmosphereis6901 K,[7]giving it the white-hued glow of an F-type star.[14]
References
[edit]- ^abcdeBrown, A. G. A.;et al. (Gaia collaboration) (2021)."GaiaEarly Data Release 3: Summary of the contents and survey properties ".Astronomy & Astrophysics.649:A1.arXiv:2012.01533.Bibcode:2021A&A...649A...1G.doi:10.1051/0004-6361/202039657.S2CID227254300.(Erratum:doi:10.1051/0004-6361/202039657e).Gaia EDR3 record for this sourceatVizieR.
- ^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,S2CID119257644.
- ^abGray, R. O.; et al. (April 2001), "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars",The Astronomical Journal,121(4): 2148–2158,Bibcode:2001AJ....121.2148G,doi:10.1086/319956.
- ^abMermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)",Catalogue of Eggen's UBV Data. SIMBAD,Bibcode:1986EgUBV........0M.
- ^abGontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system",Astronomy Letters,32(11): 759–771,arXiv:1606.08053,Bibcode:2006AstL...32..759G,doi:10.1134/S1063773706110065,S2CID119231169.
- ^Paunzen, E.; et al. (July 2014), "Investigating the possible connection between λ Bootis stars and intermediate Population II type stars",Astronomy & Astrophysics,567:8,arXiv:1406.3936,Bibcode:2014A&A...567A..67P,doi:10.1051/0004-6361/201423817,S2CID56332289,A67.
- ^abcdefgStassun, Keivan G.; et al. (September 2018), "The TESS Input Catalog and Candidate Target List",The Astronomical Journal,156(3): 102,arXiv:1706.00495,Bibcode:2018AJ....156..102S,doi:10.3847/1538-3881/aad050,ISSN0004-6256.
- ^Gáspár, András; et al. (2016), "The Correlation between Metallicity and Debris Disk Mass",The Astrophysical Journal,826(2): 171,arXiv:1604.07403,Bibcode:2016ApJ...826..171G,doi:10.3847/0004-637x/826/2/171,S2CID119241004.
- ^De Medeiros, J. R.; Alves, S.; Udry, S; Andersen, J; Nordström, B.; Mayor, M. (January 2014), "A catalog of rotational and radial velocities for evolved stars. V. Southern stars",Astronomy & Astrophysics,561:27,arXiv:1312.3474,Bibcode:2014A&A...561A.126D,doi:10.1051/0004-6361/201220762,S2CID54046583
- ^abcCasagrande, L.; et al. (2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey",Astronomy & Astrophysics,530(A138): 21,arXiv:1103.4651,Bibcode:2011A&A...530A.138C,doi:10.1051/0004-6361/201016276,S2CID56118016.
- ^"32 Tau".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2015-11-05.
- ^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,S2CID14878976.
- ^Barry, T. D.; Blatchford, J. A. (May 1931), "Occultations of stars by the moon",Astronomical Journal,41(956): 80,Bibcode:1931AJ.....41...80B,doi:10.1086/105033.
- ^"The Colour of Stars",Australia Telescope, Outreach and Education,Commonwealth Scientific and Industrial Research Organisation,December 21, 2004, archived fromthe originalon March 18, 2012,retrieved2012-01-16.
