Astronomy:Psi Tauri
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 07m 00.45697s[1] |
| Declination | +29° 00′ 04.7084″[1] |
| Apparent magnitude (V) | +5.22[2] |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | F1 V[3] |
| U−B color index | −0.01[2] |
| B−V color index | +0.34[2] |
| Astrometry | |
| Radial velocity (Rv) | +9.15±0.42[1] km/s |
| Proper motion (μ) | RA: −91.40[4] mas/yr Dec.: +7.58[4] mas/yr |
| Parallax (π) | 36.2231 ± 0.1714[1] mas |
| Distance | 90.0 ± 0.4 ly (27.6 ± 0.1 pc) |
| Absolute magnitude (MV) | 3.01[5] |
| Details | |
| Mass | 1.59[5] M☉ |
| Radius | 1.59+0.16 −0.06[1] R☉ |
| Luminosity | 5.12±0.03[1] L☉ |
| Surface gravity (log g) | 4.36±0.14[5] cgs |
| Temperature | 6885+137 −313[1] K |
| Metallicity [Fe/H] | −0.20[6] dex |
| Rotational velocity (v sin i) | 45.4±2.3[7] km/s |
| Age | 1.435[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Psi Tauri, which is Latinized from ψ Tauri, is a solitary[9] star in the zodiac constellation of Taurus. It has a yellow-white hue and is visible to the naked eye with an apparent visual magnitude of +5.22.[2] The distance to this system, as determined using an annual parallax shift of 36.2 mas as seen from the Earth,[4] is 90 light years. It is drifting further away with a radial velocity of +9 km/s.[1]
This object is an F-type main sequence star with a stellar classification of F1 V,[3] which indicates it is undergoing core hydrogen fusion. It is about 1.4 billion years old and is spinning with a projected rotational velocity of 45 km/s.[7] The star has 1.6 times the mass[5] and radius of the Sun.[1] It is radiating 4.8 times the Sun's luminosity from its photosphere at an effective temperature of 7,088 K.[5]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 Landolt, A. U. (October 1967), "Photoelectric UBV sequences in Taurus", Astronomical Journal 72: 1012–1018, doi:10.1086/110377, Bibcode: 1967AJ.....72.1012L.
- ↑ 3.0 3.1 Cowley, Anne; Fraquelli, Dorothy (February 1974), "MK Spectral Types for Some Bright F Stars", Publications of the Astronomical Society of the Pacific 86 (509): 70, doi:10.1086/129562, Bibcode: 1974PASP...86...70C.
- ↑ 4.0 4.1 4.2 van Leeuwen, F. (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.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ Holmberg, J. et al. (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.
- ↑ 7.0 7.1 Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics 542: A116, doi:10.1051/0004-6361/201118724, Bibcode: 2012A&A...542A.116A.
- ↑ "psi Tau". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=psi+Tau.
- ↑ 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.
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