| absmag_v = +0.76[3]
}}{{Starbox detail
| source =
| mass = 1.53[11]
| radius = 12[12]
| luminosity = 57.5[11]
| temperature = {{Val|4737|77|fmt=commas}}[11]
| gravity = 2.5[15]
| metal_fe = 0.12[15]
| rotational_velocity = 4.6[12]
| age_gyr = 4.21[11]
}}{{Starbox catalog
| names = {{odlist | B=ω1 Tau | F=43 Tau | BD=+19° 672 | FK5=1115 | HD=26162 | HIP=19388 | HR=1283 | SAO=93785}}[19]
}}{{Starbox reference
| Simbad = ome01+Tau
}}{{Starbox end}}Omega1 Tauri is a solitary,[20] orange hued star in the zodiac constellation of Taurus. It is faintly visible to the naked eye with an apparent visual magnitude of +5.51.[3] Based upon an annual parallax shift of 11.22 mas as seen from Earth,[ it is located about 290 light years from the Sun.]
This is an evolved K-type giant star with a stellar classification of K2 III.[3] At the estimated age of 4.2 billion years,[11] it is a red clump star that is generating energy by helium fusion at its core.[15] Omega1 Tauri has about 1.5[11] times the mass of the Sun and has expanded to around 12[12] times the Sun's radius. It is radiating 57.5 times the Sun's luminosity from its photosphere at an effective temperature of 4,737 K.[11] The radial velocity of this star shows no appreciable variation, and for this reason it is used as a radial velocity standard.[3]
References
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2. ^1 2 3 {{citation | display-authors=1 | last1=Massarotti | first1=Alessandro | last2=Latham | first2=David W. | last3=Stefanik | first3=Robert P. | last4=Fogel | first4=Jeffrey | title=Rotational and radial velocities for a sample of 761 HIPPARCOS giants and the role of binarity | journal=The Astronomical Journal | postscript=. | volume=135 | issue=1 | pages=209–231 | date=January 2008 | doi=10.1088/0004-6256/135/1/209 | bibcode=2008AJ....135..209M }}
3. ^1 2 3 4 5 6 7 {{citation | title=Abundances in the Local Region. I. G and K Giants | last1=Luck | first1=R. Earle | journal=Astronomical Journal | postscript=. | volume=150 | issue=3 | at=88 | year=2015 | bibcode=2015AJ....150...88L | doi=10.1088/0004-6256/150/3/88 |arxiv = 1507.01466 }}
4. ^1 2 3 {{citation | postscript=. | title=Red clump stars of the Milky Way - laboratories of extra-mixing | display-authors=1 | last1=Tautvaišienė | first1=G. | last2=Barisevičius | first2=G. | last3=Chorniy | first3=Y. | last4=Ilyin | first4=I. | last5=Puzeras | first5=E. | journal=Monthly Notices of the Royal Astronomical Society | volume=430 | issue=1 | pages=621−627 | date=March 2013 | doi=10.1093/mnras/sts663 | bibcode=2013MNRAS.430..621T |arxiv = 1304.4393 }}
5. ^1 2 3 4 5 6 7 8 {{citation | display-authors=1 | last1=Hekker | first1=S. | last2=Reffert | first2=S. | last3=Quirrenbach | first3=A. | last4=Mitchell | first4=D. S. | last5=Fischer | first5=D. A. | last6=Marcy | first6=G. W. | last7=Butler | first7=R. P. | title=Precise radial velocities of giant stars. I. Stable stars | journal=Astronomy and Astrophysics | volume=454 | issue=3 | pages=943–949 | date=August 2006 | doi=10.1051/0004-6361:20064946 | bibcode=2006A&A...454..943H | arxiv=astro-ph/0604502 | postscript=. }}
6. ^1 {{cite simbad | title=ome01 Tau | accessdate=2017-06-30 | postscript=. }}