132 Tauri

132 Tauri is a binary star[2] system in the constellation Taurus. It is faintly visible to the naked eye with an apparent visual magnitude of 4.89.[2] Based upon a poorly-constrained annual parallax shift of 8.97±1.98 mas,[1] it is located roughly 360 light years from the Sun. The system is moving further away with a heliocentric radial velocity of +16 km/s.[5] It lies near the ecliptic and thus is subject to occultation by the Moon. One such event was observed September 3, 1991.[8]

132 Tauri
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 05h 49m 00.96598s[1]
Declination +24° 34′ 03.1220″[1]
Apparent magnitude (V) 4.89 (5.07 + 9.09)[2]
Characteristics
Spectral type G9 III[3]
B−V color index 1.021[4]
Astrometry
Radial velocity (Rv)+15.8±0.6[5] km/s
Proper motion (μ) RA: +10.44[1] mas/yr
Dec.: −8.30[1] mas/yr
Parallax (π)8.97 ± 1.98[1] mas
Distanceapprox. 360 ly
(approx. 110 pc)
Details
132 Tau Aa
Surface gravity (log g)2.74±0.11[6] cgs
Temperature4,853±47[6] K
Metallicity [Fe/H]0.18±0.05[6] dex
Other designations
132 Tau, BD+24° 970, FK5 2435, HD 38751, HIP 27468, HR 2002, SAO 77592, WDS J05490+2434AB[7]
Database references
SIMBADdata

This system forms a wide double star with an angular separation of 3.8″ along a position angle of 230°, as of 1991. The brighter star, component A, has an apparent magnitude of 4.99 while the fainter secondary, component B, is of magnitude 9.09. The primary is itself an unresolved binary[9] with a combined stellar classification of G9 III,[3] which matches an aging G-type giant star that has exhausted the hydrogen at its core and evolved away from the main sequence.

References
  1. 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.
  2. 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.
  3. Keenan, Philip C.; Barnbaum, Cecilia (June 1999), "Revision and Calibration of MK Luminosity Classes for Cool Giants by HIPPARCOS Parallaxes", The Astrophysical Journal, 518 (2): 859–865, Bibcode:1999ApJ...518..859K, doi:10.1086/307311.
  4. 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.
  5. de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, A61.
  6. Prugniel, Ph.; et al. (July 2011), "The atmospheric parameters and spectral interpolator for the MILES stars", Astronomy & Astrophysics, 531: A165, arXiv:1104.4952, Bibcode:2011A&A...531A.165P, doi:10.1051/0004-6361/201116769.
  7. "132 Tau". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-03-27.
  8. Meyer, C.; et al. (April 1995), "Observations of lunar occultations at Observatoire de la Cote d'Azur", Astronomy and Astrophysics Supplement, 110: 107, Bibcode:1995A&AS..110..107M
  9. Mason, B. D.; et al. (2014), The Washington Visual Double Star Catalog, Bibcode:2001AJ....122.3466M, doi:10.1086/323920
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