| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 05h 24m 25.46328s[2] |
| Declination | +17° 23′ 00.7264″[2] |
| Apparent magnitude (V) | 5.0[3] |
| Characteristics | |
| A | |
| Spectral type | F8 V[4] |
| U−B color index | −0.05[5] |
| B−V color index | 0.544[6] |
| Variable type | BY Dra[5] |
| B | |
| Spectral type | K5 V[4] |
| Astrometry | |
| A | |
| Radial velocity (Rv) | +37.8[7] km/s |
| Proper motion (μ) | RA: +250.585[2] mas/yr Dec.: −7.156[2] mas/yr |
| Parallax (π) | 68.5908 ± 0.1040 mas[2] |
| Distance | 47.55 ± 0.07 ly (14.58 ± 0.02 pc) |
| Absolute magnitude (MV) | 3.49 ± 0.06[3] |
| Details | |
| 111 Tau A | |
| Mass | 1.08[3] M☉ |
| Radius | 1.67 ± 0.06[3] R☉ |
| Luminosity | 1.845[8] L☉ |
| Surface gravity (log g) | 4.24[9] cgs |
| Temperature | 6,015[9] K |
| Metallicity [Fe/H] | −0.14[9] dex |
| Rotation | 3.503±0.006 d[10] |
| Rotational velocity (v sin i) | 16.0[11] km/s |
| Age | 20–50[12] Myr |
| Other designations | |
| 111 Tau A: Gl 202, HR 1780, BD+17°920, HD 35296, SAO 94526, HIP 25278, V1119 Tau | |
| 111 Tau B: Gl 201, BD+17°917, HD 35171, SAO 94513, HIP 25220 | |
| Database references | |
| SIMBAD | A |
| B | |
111 Tauri is a wide binary star[4] system in the constellation Taurus. It is located at a distance of 48 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.[4] The primary 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 5.0 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.[9][13] This star shows an unusually high content of lithium, which remains unexplained.[13] Age estimates for this star range from 3.6 to 3.76 billion years.[7][14] however the most recent age determination indicates a very young star with an age of 20 to 50 million years.[12] It is a prominent X-ray source.[13]
This star is rotating relatively rapidly, completing a rotation along the equator every 3.5 days[10] as compared to 25 days for the Sun. It is also undergoing differential rotation in which the rotation velocity varies by latitude.[15] 111 Tauri is a BY Draconis variable, and has been given the variable star designation V1119 Tauri.[16]
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.[14] The space velocity components of this star are [U, V, W] = [−36.94, −14.63, 7.63] km/s.[17] It is a member of the Hyades stellar kinematic group of co-moving stars.[13]
References
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d 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
- ^ a b c d 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. S2CID 14878976.
- ^ a b c "V* V1119 Tau -- Variable of BY Dra". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2011-07-03.
- ^ 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. S2CID 18759600.
- ^ a b 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. S2CID 118577511.
- ^ 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.
- ^ a b c d 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 (3): 491–506. arXiv:astro-ph/9912342. Bibcode:2000A&AS..141..491C. doi:10.1051/aas:2000124. S2CID 16273589.
- ^ a b Hempelmann, A.; et al. (2016). "Measuring rotation periods of solar-like stars using TIGRE. A study of periodic CaII H+K S-index variability". Astronomy and Astrophysics. 586. A14. Bibcode:2016A&A...586A..14H. doi:10.1051/0004-6361/201526972.
- ^ Schröder, C.; Reiners, Ansgar; Schmitt, Jürgen H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377[permanent dead link]
- ^ a b Waite, I. A.; et al. (2015). "Magnetic fields on young, moderately rotating Sun-like stars – I. HD 35296 and HD 29615". Monthly Notices of the Royal Astronomical Society. 449 (1): 8–24. arXiv:1502.05788. Bibcode:2015MNRAS.449....8W. doi:10.1093/mnras/stv006.
- ^ a b c d 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. S2CID 17811620.
- ^ a b 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. S2CID 54940779.
- ^ Reiners, Ansgar (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, S2CID 8642707
- ^ "V1119 Tau". The International Variable Star Index. AAVSO. Retrieved 27 June 2022.
- ^ 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. S2CID 55727428.
This page was last edited on 24 September 2023, at 22:40