Omega Persei

Omega Persei

Location of ω Persei (circled)
Observation data Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation	Perseus
Right ascension	03^h 11^m 17.38161^s[1]
Declination	+39° 36′ 41.7014″[1]
Apparent magnitude (V)	+4.614[2]
Characteristics
Evolutionary stage	red clump[3]
Spectral type	K0 III[2]
B−V color index	1.122[2]
Astrometry
Radial velocity (Rv)	6.61[2] km/s
Proper motion (μ)	RA: −26.26[1] mas/yr Dec.: +5.40[1] mas/yr
Parallax (π)	11.32 ± 0.23 mas[1]
Distance	288 ± 6 ly (88 ± 2 pc)
Absolute magnitude (MV)	−0.234[4]
Details
Mass	2.04[2] M☉
Radius	19[5] R☉
Luminosity	144.5[2] L☉
Surface gravity (log g)	2.5[5] cgs
Temperature	4,586±18[2] K
Metallicity [Fe/H]	−0.10[4] dex
Rotational velocity (v sin i)	3.3[5] km/s
Age	1.65[2] Gyr
Other designations
ω Per, 28 Persei, BD+39° 724, FK5 2667, HD 19656, HIP 14817, HR 947, SAO 56224, WDS J03113+3937A[6]
Database references
SIMBAD	data

Omega Persei (ω Persei) is a solitary,^[7] orange-hued star in the northern constellation of Perseus. The star is faintly visible to the naked eye with an apparent visual magnitude of +4.6.^[2] Based upon an annual parallax shift of 11.32 mas as seen from the Earth,^[1] the star is about 288 light years from the Sun.

ω Persei has the traditional name Gorgonea Quarta /ɡɔːrɡəˈniːə ˈkwɔːrtə/, being the fourth member of the quartet called the Gorgonea in reference to the Gorgons from the legend of Perseus.^[8]

This is an evolved K-type giant star with a stellar classification of K0 III.^[2] It is a red clump star that is generating energy via helium fusion at its core.^[3] At the estimated age of 1.65 billion years, Omega Persei has double^[2] times the mass of the Sun and has expanded to about 19^[5] times the Sun's radius. It is radiating 144.5 times the Sun's luminosity from its photosphere at an effective temperature of 4,586 K.^[2]

References

1. van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
2. Luck, R. Earle (September 2015), "Abundances in the Local Region. I. G and K Giants", The Astronomical Journal, 150 (3): 23, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID 118505114, 88.
3. Alves, David R. (August 2000), "K-Band Calibration of the Red Clump Luminosity", The Astrophysical Journal, 539 (2): 732–741, arXiv:astro-ph/0003329, Bibcode:2000ApJ...539..732A, doi:10.1086/309278, S2CID 16673121.
4. Soubiran, C.; et al. (2008), "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants", Astronomy and Astrophysics, 480 (1): 91–101, arXiv:0712.1370, Bibcode:2008A&A...480...91S, doi:10.1051/0004-6361:20078788, S2CID 16602121.
5. Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209, S2CID 121883397.
6. "ome Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-06-19.
7. 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
8. Allen, Richard Hinckley (1899), Star-names and their meanings, G. E. Stechert, p. 334