Astronomy:109 Tauri
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Taurus |
| Right ascension | 05h 19m 16.60169s[1] |
| Declination | +22° 05′ 47.3740″[1] |
| Apparent magnitude (V) | 4.96[2] |
| Characteristics | |
| Spectral type | G8 III[3] |
| B−V color index | 0.937±0.001[2] |
| Astrometry | |
| Radial velocity (Rv) | +19.03±0.01[4] km/s |
| Proper motion (μ) | RA: +18.91[1] mas/yr Dec.: −81.57[1] mas/yr |
| Parallax (π) | 13.19 ± 0.30[1] mas |
| Distance | 247 ± 6 ly (76 ± 2 pc) |
| Absolute magnitude (MV) | 0.56[2] |
| Details[4] | |
| Mass | 2.47±0.08 M☉ |
| Radius | 8.14±0.46 R☉ |
| Luminosity | 60+10 −12 L☉ |
| Surface gravity (log g) | 2.96±0.01 cgs |
| Temperature | 5,035±23 K |
| Metallicity [Fe/H] | 0.10±0.04 dex |
| Rotational velocity (v sin i) | 1.15±0.62 km/s |
| Age | 600±50 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
109 Tauri, or n Tauri, is a single,[6] yellow-hued star in the zodiac constellation of Taurus. It has an apparent visual magnitude of 4.96[2] and is faintly visible to the naked eye. The star has an annual parallax shift of 13.19±0.30 mas,[1] putting it around 247 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.24 due to interstellar dust.[4] It is moving further from the Sun with a heliocentric radial velocity of +19 km/s.[4]
This is an evolved giant star with a stellar classification of G8 III,[3] having consumed the hydrogen at its core and moved off the main sequence. At the age of 600[4] million years, it has become a red clump giant, indicating that it is on the horizontal branch and is generating energy through helium fusion at its core.[7] The star has an estimated 2.47 times the mass of the Sun and has expanded to around eight times the Sun's radius. It is radiating about 60 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,035 K.[4]
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 2.3 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 Roman, Nancy G. (July 1952), "The Spectra of the Bright Stars of Types F5-K5", Astrophysical Journal 116: 122, doi:10.1086/145598, Bibcode: 1952ApJ...116..122R.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Jofré, E. et al. (February 2015), "Stellar parameters and chemical abundances of 223 evolved stars with and without planets", Astronomy & Astrophysics 574: 46, doi:10.1051/0004-6361/201424474, A50, Bibcode: 2015A&A...574A..50J.
- ↑ "109 Tau". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=109+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.
- ↑ Puzeras, E. et al. (October 2010), "High-resolution spectroscopic study of red clump stars in the Galaxy: iron-group elements", Monthly Notices of the Royal Astronomical Society 408 (2): 1225–1232, doi:10.1111/j.1365-2966.2010.17195.x, Bibcode: 2010MNRAS.408.1225P.
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