39 Tauri
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 04h 05m 20.258s[1]
Declination +22° 00′ 32.06″[1]
Apparent magnitude (V) 5.90[2]
Characteristics
Spectral type G5 V[3]
U−B color index +0.12[4]
B−V color index +0.62[4]
Astrometry
Radial velocity (Rv)+24.0±0.1[5] km/s
Proper motion (μ) RA: +172.212 mas/yr[1]
Dec.: −130.609 mas/yr[1]
Parallax (π)59.4728 ± 0.0361 mas[1]
Distance54.84 ± 0.03 ly
(16.81 ± 0.01 pc)
Details
Mass1.10±0.10[2] M☉
Radius0.96±0.07[2] R☉
Luminosity1.01[2] L☉
Surface gravity (log g)4.52±0.09[2] cgs
Temperature5,903±36[2] K
Metallicity [Fe/H]0.14±0.03[2] dex
Rotation9.12[5] d
Rotational velocity (v sin i)5.52[6] km/s
Age1.0[2] Gyr
Other designations
39 Tau, BD+21 587, GJ 160, HD 25680, HIP 19076, HR 1262, SAO 76438[7]
Database references
SIMBADdata
ARICNSdata

39 Tauri is a binary star in the northern constellation of Taurus. It has an apparent visual magnitude of 5.90, so, according to the Bortle scale, it is faintly visible from suburban skies at night. Measurements made with the Hipparcos spacecraft show an annual parallax shift of 0.0594728″, which is equivalent to a distance of around 55 light years from the Sun.

A light curve for 39 Tauri, plotted from Kepler (K2) data[8]

39 Tauri has been resolved into a pair of stars using speckle interferometry.[9] However, many observations have failed to resolve the secondary star.[10]

A stellar classification of G5 V[3] matches that of a G-type main sequence star; the type of the secondary component is unknown. Stellar models indicate the primary component is similar in physical properties to the Sun, with 110% of the Sun's mass, 96% of the radius, and shining with almost the same luminosity.[2] The overall metallicity of the star—the abundance of elements other than hydrogen and helium—is similar to the Sun.[11] At a relatively youthful estimated age of one billion years,[2] it is rotating with a period of 9.12[5] days. Based upon Hipparcos data, it displays a mild variability with an amplitude of 0.06 magnitude.[12]

The space velocity components of 39 Tauri are: –25.0(U), –14.0(V), –6.0(W). The surface activity and kinematic properties of this star are consistent with membership in the IC 2391 moving group.[13] It is following an orbit through the Milky Way galaxy that has an eccentricity of 0.06 carrying it as close as 23.9 kly (7.34 kpc) to the Galactic Center, and as far away as 26.8 kly (8.21 kpc). The orbital inclination will carry the star no further than 33 ly (10 pc) away from the galactic plane.[11]

References

  1. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 4 5 6 7 8 9 10 Ghezzi, L.; et al. (September 2010), "Stellar Parameters and Metallicities of Stars Hosting Jovian and Neptunian Mass Planets: A Possible Dependence of Planetary Mass on Metallicity", The Astrophysical Journal, 720 (2): 1290–1302, arXiv:1007.2681, Bibcode:2010ApJ...720.1290G, doi:10.1088/0004-637X/720/2/1290, S2CID 118565025.
  3. 1 2 Shenavrin, V. I.; et al. (January 2011), "Search for and study of hot circumstellar dust envelopes", Astronomy Reports, 55 (1): 31–81, Bibcode:2011ARep...55...31S, doi:10.1134/S1063772911010070, S2CID 122700080.
  4. 1 2 Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
  5. 1 2 3 López-Santiago, J.; et al. (May 2010), "A high-resolution spectroscopic survey of late-type stars: chromospheric activity, rotation, kinematics, and age", Astronomy and Astrophysics, 515: A97, arXiv:1002.1663, Bibcode:2010A&A...514A..97L, doi:10.1051/0004-6361/200913437, S2CID 118640516.
  6. ↑ Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter", Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725, S2CID 43455849.
  7. ↑ "39 Tau". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2013-10-13.
  8. ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, retrieved 19 September 2022.
  9. ↑ Hartkopf, William I.; Mason, Brian D. (September 2009), "Speckle Interferometry at Mount Wilson Observatory: Observations Obtained in 2006-2007 and 35 New Orbits", The Astronomical Journal, 138 (3): 813–826, Bibcode:2009AJ....138..813H, doi:10.1088/0004-6256/138/3/813.
  10. ↑ Roberts, Lewis C. Jr.; et al. (November 2005), "Adaptive Optics Photometry and Astrometry of Binary Stars", The Astronomical Journal, 130 (5): 2262–2271, Bibcode:2005AJ....130.2262R, doi:10.1086/491586.
  11. 1 2 Casagrande, L.; et al. (June 2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy and Astrophysics, 530: A138, arXiv:1103.4651, Bibcode:2011A&A...530A.138C, doi:10.1051/0004-6361/201016276, S2CID 56118016.
  12. ↑ Adelman, S. J.; et al. (December 2000), "On the Variability of G0-G9 Stars", Information Bulletin on Variable Stars, 4993: 1, Bibcode:2000IBVS.4993....1A.
  13. ↑ Murgas, F.; et al. (April 2013), "Stellar activity as a tracer of moving groups", Astronomy and Astrophysics, 552: A27, arXiv:1302.6935, Bibcode:2013A&A...552A..27M, doi:10.1051/0004-6361/201219483, S2CID 7621053.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.