Astronomy:111 Tauri

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Short description: Wide binary star system in the constellation Taurus
111 Tauri
V1119TauLightCurve.png
A light curve for V1119 Tauri, plotted from TESS data[1]
Observation data
Equinox J2000.0]] (ICRS)
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[2] mas
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. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 3.3 Fuhrmann, Klaus (February 2008), "Nearby stars of the Galactic disc and halo - IV", Monthly Notices of the Royal Astronomical Society 384 (1): 173–224, doi:10.1111/j.1365-2966.2007.12671.x, Bibcode: 2008MNRAS.384..173F 
  4. ↑ 4.0 4.1 4.2 4.3 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. doi:10.1111/j.1365-2966.2008.13596.x. Bibcode: 2008MNRAS.389..869E. 
  5. ↑ 5.0 5.1 5.2 "V* V1119 Tau -- Variable of BY Dra". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=111+Tauri. Retrieved 2011-07-03. 
  6. ↑ van Leeuwen, F. (November 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. 
  7. ↑ 7.0 7.1 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. doi:10.1051/0004-6361/200811191. Bibcode: 2009A&A...501..941H. 
  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. doi:10.1093/pasj/59.2.335. Bibcode: 2007PASJ...59..335T. 
  9. ↑ 9.0 9.1 9.2 9.3 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. doi:10.1051/aas:2000124. Bibcode: 2000A&AS..141..491C. 
  10. ↑ 10.0 10.1 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. doi:10.1051/0004-6361/201526972. Bibcode: 2016A&A...586A..14H. https://www.aanda.org/articles/aa/full_html/2016/02/aa26972-15/aa26972-15.html. 
  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", Astronomy and Astrophysics 493 (3): 1099–1107, doi:10.1051/0004-6361:200810377, Bibcode: 2009A&A...493.1099S, http://goedoc.uni-goettingen.de/goescholar/bitstream/handle/1/9690/aa10377-08.pdf?sequence=2 [yes|permanent dead link|dead link}}]
  12. ↑ 12.0 12.1 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. doi:10.1093/mnras/stv006. Bibcode: 2015MNRAS.449....8W. 
  13. ↑ 13.0 13.1 13.2 13.3 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. doi:10.1086/591638. Bibcode: 2008ApJ...687..566M. 
  14. ↑ 14.0 14.1 Trilling, D. E. (February 2008). "Debris Disks around Sun-like Stars". The Astrophysical Journal 674 (2): 1086–1105. doi:10.1086/525514. Bibcode: 2008ApJ...674.1086T. 
  15. ↑ Reiners, Ansgar (January 2006), "Rotation- and temperature-dependence of stellar latitudinal differential rotation", Astronomy and Astrophysics 446 (1): 267–277, doi:10.1051/0004-6361:20053911, Bibcode: 2006A&A...446..267R 
  16. ↑ "V1119 Tau". AAVSO. https://www.aavso.org/vsx/index.php?view=detail.top&oid=36136. 
  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. doi:10.1046/j.1365-8711.2001.04781.x. Bibcode: 2001MNRAS.328...45M. 



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