Astronomy:75 Tauri
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 28m 26.37004s[1] |
| Declination | +16° 21′ 34.8231″[1] |
| Apparent magnitude (V) | 4.96[2] |
| Characteristics | |
| Spectral type | K1 IIIb[2] |
| B−V color index | 1.137[3] |
| Astrometry | |
| Radial velocity (Rv) | +16.24±0.20[4] km/s |
| Proper motion (μ) | RA: +7.91[1] mas/yr Dec.: +18.14[1] mas/yr |
| Parallax (π) | 17.47 ± 0.42[1] mas |
| Distance | 187 ± 4 ly (57 ± 1 pc) |
| Absolute magnitude (MV) | 1.18[3] |
| Details[3] | |
| Mass | 1.53±0.23 M☉ |
| Radius | 11[5] R☉ |
| Luminosity | 40.74+2.02 −1.92 L☉ |
| Surface gravity (log g) | 2.81±0.28 cgs |
| Temperature | 4,697±60 K |
| Metallicity [Fe/H] | −0.08±0.11 dex |
| Rotational velocity (v sin i) | 2.5[5] km/s |
| Age | 2.7+1.0 −1.5 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
75 Tauri is a single,[7] orange-hued star in the zodiac of constellation Taurus. It is a dim star but visible to the naked eye with an apparent visual magnitude of 4.96.[2] Based upon an annual parallax shift of 17.47 mas as seen from Earth's orbit, it is located around 187 light years away. Due to its position near the ecliptic, it is subject to lunar occultations.[8] The star is moving further from the Sun with a heliocentric radial velocity of +16 km/s.[4]
The stellar classification of 75 Tauri is K1 IIIb,[2] indicating it is an aging giant star that has exhausted the supply of hydrogen at its core. At the estimated age of roughly 2.7 billion years,[3] this has become a red clump star that is generating energy through helium fusion in its core region.[9] The star has 1.5 times the mass of the Sun and has expanded to 11 times the Sun's radius. It is radiating 41 times the Sun's luminosity from its enlarged photosphere at an effective temperature of around 4,697 K.[3]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 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 2.3 Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series 71: 245, doi:10.1086/191373, Bibcode: 1989ApJS...71..245K.
- ↑ 3.0 3.1 3.2 3.3 3.4 Da Silva, Ronaldo et al. (2015), "Homogeneous abundance analysis of FGK dwarf, subgiant, and giant stars with and without giant planets", Astronomy & Astrophysics 580: A24, doi:10.1051/0004-6361/201525770, Bibcode: 2015A&A...580A..24D.
- ↑ 4.0 4.1 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.
- ↑ 5.0 5.1 Massarotti, Alessandro et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal 135 (1): 209–231, doi:10.1088/0004-6256/135/1/209, Bibcode: 2008AJ....135..209M.
- ↑ "75 Tau". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=75+Tau.
- ↑ 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.
- ↑ Evans, D. S.; Edwards, D. A. (August 1981), "Photoelectric observations of lunar occultations. XII", Astronomical Journal 86: 1277−1287, doi:10.1086/113008, Bibcode: 1981AJ.....86.1277E.
- ↑ Tautvaišienė, G. et al. (December 2010), "C, N and O abundances in red clump stars of the Milky Way", Monthly Notices of the Royal Astronomical Society 409 (3): 1213–1219, doi:10.1111/j.1365-2966.2010.17381.x, Bibcode: 2010MNRAS.409.1213T.
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