111 Tauri
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 05h 24m 25.46380s[1] |
| Declination | +17° 23′ 00.7166″[1] |
| Apparent magnitude (V) | 5.1149[1] |
| Characteristics | |
| Spectral type | F8 V + K5 V[2] |
| U−B color index | −0.05[3] |
| B−V color index | 0.544[1] |
| Variable type | BY Dra[3] |
| Astrometry | |
| Radial velocity (Rv) | +37.8[4] km/s |
| Proper motion (μ) | RA: +251.05[1] mas/yr Dec.: −7.99[1] mas/yr |
| Parallax (π) | 69.51 ± 0.38[1] mas |
| Distance | 46.9 ± 0.3 ly (14.39 ± 0.08 pc) |
| Absolute magnitude (MV) | 3.49 ± 0.06[5] |
| Details | |
| 111 Tau A | |
| Mass | 1.08[5] M☉ |
| Radius | 1.67 ± 0.06[5] R☉ |
| Luminosity | 1.845[6] L☉ |
| Surface gravity (log g) | 4.24[7] cgs |
| Temperature | 6,015[7] K |
| Metallicity [Fe/H] | −0.14[7] dex |
| Rotation | 4.1 days[8] |
| Rotational velocity (v sin i) | 16.0[9] km/s |
| Age | 3.76[10] Gyr |
| Other designations | |
111 Tauri is a wide binary star[2] system in the constellation Taurus. It is located at a distance of about 47 light years from the Sun. Primary component A is a main sequence star with a stellar classification of F8V. The secondary component B (Gliese 201) is a K-type main sequence star.[2] It is larger and more luminous than the Sun, with about 130% of the Sun's radius and 185% of the Sun's luminosity. The apparent magnitude of 5.1 indicates it is a faint star that can be viewed by the naked eye under good, dark-sky conditions.
The metallicity of the primary star, which measures the proportion of elements other than hydrogen and helium, is similar to the Sun. Estimates of [Fe/H], which is the logarithm of the ratio of iron to hydrogen as compared to the Sun, range from a low of −0.14 to a high of 0.05.[7][8] This star shows an unusually high content of Lithium, which remains unexplained.[8] Age estimates for this star range from 3.6 to 3.76 billion years.[4][10] It is a prominent X-ray source.[8]
This star is rotating relatively rapidly, completing a rotation along the equator every 4.1 days as compared to 25 days for the Sun. It is also undergoing differential rotation in which the rotation velocity varies by latitude.[11]
This star was examined for an excess of infrared emission that could indicate it has a circumstellar debris disk of dust, but no significant excess was observed.[10] The space velocity components of this star are [U, V, W] = [−36.94, −14.63, 7.63] km/s.[12] It shares a common proper motion with HIP 25220, an active star with stellar classification K4V. Both stars are members of the Hyades stellar kinematic group of co-moving stars.[8]
References
- 1 2 3 4 5 6 7 van Leeuwen, F. (November 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. - 1 2 3 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.
- 1 2 3 "V* V1119 Tau -- Variable of BY Dra". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2011-07-03.
- 1 2 Holmberg, J.; Nordstrom, B.; Andersen, J. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics. 501 (3): 941–947. arXiv:0811.3982. Bibcode:2009A&A...501..941H. doi:10.1051/0004-6361/200811191.
- 1 2 3 Fuhrmann, Klaus (February 2008), "Nearby stars of the Galactic disc and halo - IV", Monthly Notices of the Royal Astronomical Society, 384 (1): 173–224, Bibcode:2008MNRAS.384..173F, doi:10.1111/j.1365-2966.2007.12671.x
- ↑ Takeda, Yoichi (April 2007). "Fundamental Parameters and Elemental Abundances of 160 F-G-K Stars Based on OAO Spectrum Database". Publications of the Astronomical Society of Japan. 59 (2): 335–356. Bibcode:2007PASJ...59..335T. doi:10.1093/pasj/59.2.335.
- 1 2 3 4 Chen, Y. Q.; Nissen, P. E.; Zhao, G.; Zhang, H. W.; Benoni, T. (February 2000). "Chemical composition of 90 F and G disk dwarfs". Astronomy and Astrophysics Supplement. 141: 491–506. arXiv:astro-ph/9912342. Bibcode:2000A&AS..141..491C. doi:10.1051/aas:2000124.
- 1 2 3 4 5 Makarov, V. V.; Zacharias, N.; Hennessy, G. S. (November 2008). "Common Proper Motion Companions to Nearby Stars: Ages and Evolution". The Astrophysical Journal. 687 (1): 566–578. arXiv:0808.3414. Bibcode:2008ApJ...687..566M. doi:10.1086/591638.
- ↑ Schröder, C.; Reiners, A.; Schmitt, J. H. M. M. (January 2009). "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo". Astronomy and Astrophysics. 493 (3): 1099–1107. Bibcode:2009A&A...493.1099S. doi:10.1051/0004-6361:200810377.
- 1 2 3 Trilling, D. E.; et al. (February 2008). "Debris Disks around Sun-like Stars". The Astrophysical Journal. 674 (2): 1086–1105. arXiv:0710.5498. Bibcode:2008ApJ...674.1086T. doi:10.1086/525514.
- ↑ Reiners, A. (January 2006). "Rotation- and temperature-dependence of stellar latitudinal differential rotation". Astronomy and Astrophysics. 446 (1): 267–277. arXiv:astro-ph/0509399. Bibcode:2006A&A...446..267R. doi:10.1051/0004-6361:20053911.
- ↑ Montes, D.; et al. (November 2001). "Late-type members of young stellar kinematic groups - I. Single stars". Monthly Notices of the Royal Astronomical Society. 328 (1): 45–63. arXiv:astro-ph/0106537. Bibcode:2001MNRAS.328...45M. doi:10.1046/j.1365-8711.2001.04781.x.