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 55light years from the Sun.
A light curve for 39 Tauri, plotted from Kepler (K2) data[8]
Star in the constellation Taurus
This article is about A2 Tauri. For other stars with this Bayer designation, see A Tauri.
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 G5V[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 0.06magnitude.[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 23.9kly (7.34kpc) to the Galactic Center, and as far away as 26.8kly (8.21kpc). The orbital inclination will carry the star no further than 33ly (10pc) away from the galactic plane.[11]
Ghezzi, L.; etal. (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, S2CID118565025.
Johnson, H. L.; etal. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99), Bibcode:1966CoLPL...4...99J.
López-Santiago, J.; etal. (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, S2CID118640516.
Martínez-Arnáiz, R.; etal. (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, S2CID43455849.
"39 Tau". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2013-10-13.
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.
Roberts, Lewis C., Jr.; etal. (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.
Casagrande, L.; etal. (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, S2CID56118016.
Adelman, S. J.; etal. (December 2000), "On the Variability of G0-G9 Stars", Information Bulletin on Variable Stars, 4993: 1, Bibcode:2000IBVS.4993....1A.
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