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111 Tauri

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111 Tauri

A light curve for V1119 Tauri, plotted from TESS data[1]
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]
Distance47.55 ± 0.07 ly
(14.58 ± 0.02 pc)
Absolute magnitude (MV)3.49 ± 0.06[3]
Details
111 Tau A
Mass1.08[3] M☉
Radius1.67 ± 0.06[3] R☉
Luminosity1.845[8] L☉
Surface gravity (log g)4.24[9] cgs
Temperature6,015[9] K
Metallicity [Fe/H]−0.14[9] dex
Rotation3.503±0.006 d[10]
Rotational velocity (v sin i)16.0[11] km/s
Age20–50[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
SIMBADA
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

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ 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.
  3. ^ 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
  4. ^ 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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  5. ^ a b c "V* V1119 Tau -- Variable of BY Dra". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2011-07-03.
  6. ^ 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.
  7. ^ 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.
  8. ^ 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.
  9. ^ 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.
  10. ^ 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.
  11. ^ 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
  12. ^ 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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  13. ^ 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.
  14. ^ 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.
  15. ^ 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
  16. ^ "V1119 Tau". The International Variable Star Index. AAVSO. Retrieved 27 June 2022.
  17. ^ 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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
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