Astronomy:132 Tauri
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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 |
| Distance | approx. 360 ly (approx. 110 pc) |
| Details | |
| 132 Tau Aa | |
| Surface gravity (log g) | 2.74±0.11[6] cgs |
| Temperature | 4,853±47[6] K |
| Metallicity [Fe/H] | 0.18±0.05[6] dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
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]
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
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ 3.0 3.1 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, doi:10.1086/307311, Bibcode: 1999ApJ...518..859K.
- ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 5.0 5.1 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, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
- ↑ 6.0 6.1 6.2 Prugniel, Ph. et al. (July 2011), "The atmospheric parameters and spectral interpolator for the MILES stars", Astronomy & Astrophysics 531: A165, doi:10.1051/0004-6361/201116769, Bibcode: 2011A&A...531A.165P.
- ↑ "132 Tau". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=132+Tau.
- ↑ 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
- ↑ Mason, B. D. et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal 122 (6): 3466, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M
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