Astronomy:32 Tauri

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Short description: Yellow-white hued subgiant star in the constellation Taurus.
32 Tauri
Taurus constellation map.svg
Red circle.svg
Location of 32 Tauri (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Taurus
Right ascension  03h 56m 52.077s[1]
Declination +22° 28′ 40.70″[1]
Apparent magnitude (V) 5.62[2]
Characteristics
Spectral type F2IVs[3]
U−B color index +0.00[4]
B−V color index +0.345±0.004[2]
Astrometry
Radial velocity (Rv)+31.90[5] km/s
Proper motion (μ) RA: +70.674[1] mas/yr
Dec.: −114.026[1] mas/yr
Parallax (π)22.5957 ± 0.0385[1] mas
Distance144.3 ± 0.2 ly
(44.26 ± 0.08 pc)
Absolute magnitude (MV)2.42[6]
Details
Mass2.04[7] M☉
Radius2.75[7] R☉
Luminosity15.4[7] L☉
Surface gravity (log g)3.87[7] cgs
Temperature6.901[7] K
Metallicity [Fe/H]−0.19[8] dex
Rotational velocity (v sin i)19.7[9] km/s
Age2.1[10] Gyr
Other designations
BD+22°605, FK5 2283, HD 24740, HIP 18471, HR 1218, SAO 76339, Ross 33.[11]
Database references
SIMBADdata

32 Tauri is the Flamsteed designation for a solitary[12] star in the zodiac constellation of Taurus. It has a visual magnitude of 5.64,[4] making it visible to the naked eye from suburban skies (according to the Bortle scale). The position of this star near the ecliptic plane means that it is subject to occultations by the Moon.[13] Parallax measurements put it at a distance of 144 light years from the Sun.[1] It is drifting further away with a radial velocity of +31.9[5] km/s, having come to within 88.9 light-years some 759,000 years ago.[2]

The spectrum of this star matches a stellar classification of F2IVs,[3] with the luminosity class of IV indicating that this star has reached the subgiant stage and is in the process of evolving into a giant star. It has twice the mass of the sun with nearly three times the Sun'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] The effective temperature of the star's outer atmosphere is 6901 K,[7] giving it the white-hued glow of an F-type star.[14]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  3. ↑ 3.0 3.1 Gray, 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, doi:10.1086/319956, Bibcode: 2001AJ....121.2148G. 
  4. ↑ 4.0 4.1 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode: 1986EgUBV........0M. 
  5. ↑ 5.0 5.1 Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system", Astronomy Letters 32 (11): 759–771, doi:10.1134/S1063773706110065, Bibcode: 2006AstL...32..759G. 
  6. ↑ Paunzen, E. et al. (July 2014), "Investigating the possible connection between λ Bootis stars and intermediate Population II type stars", Astronomy & Astrophysics 567: 8, doi:10.1051/0004-6361/201423817, A67, Bibcode: 2014A&A...567A..67P. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 Stassun, Keivan G. et al. (September 2018), "The TESS Input Catalog and Candidate Target List", The Astronomical Journal 156 (3): 102, doi:10.3847/1538-3881/aad050, ISSN 0004-6256, Bibcode: 2018AJ....156..102S. 
  8. ↑ Gáspár, András et al. (2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal 826 (2): 171, doi:10.3847/0004-637x/826/2/171, Bibcode: 2016ApJ...826..171G. 
  9. ↑ 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, doi:10.1051/0004-6361/201220762, Bibcode: 2014A&A...561A.126D 
  10. ↑ 10.0 10.1 10.2 Casagrande, 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, doi:10.1051/0004-6361/201016276, Bibcode: 2011A&A...530A.138C. 
  11. ↑ "32 Tau". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=32+Tau. 
  12. ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  13. ↑ Barry, T. D.; Blatchford, J. A. (May 1931), "Occultations of stars by the moon", Astronomical Journal 41 (956): 80, doi:10.1086/105033, Bibcode: 1931AJ.....41...80B. 
  14. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html, retrieved 2012-01-16. 



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