Gamma Comae Berenices

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γ Comae Berenices
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Coma Berenices
Right ascension 12h 26m 56.27207s[1]
Declination +28° 16′ 06.3211″[1]
Apparent magnitude (V) 4.36[2]
Spectral type K1 III Fe0.5[3]
U−B color index +1.16[2]
B−V color index +1.13[2]
R−I color index +0.51[4]
Radial velocity (Rv) +3.38±0.11[5] km/s
Proper motion (μ) RA: −83.95[1] mas/yr
Dec.: −81.13[1] mas/yr
Parallax (π) 19.50 ± 0.19[1] mas
Distance 167 ± 2 ly
(51.3 ± 0.5 pc)
Absolute magnitude (MV) 0.76[6]
Mass 1.65±0.18 M
Radius 11.76±0.14 R
Luminosity 58.2±1.1 L
Surface gravity (log g) 0.16±0.10 cgs
Temperature 4,652±18 K
Metallicity [Fe/H] 0.16±0.10 dex
Rotational velocity (v sin i) ≤ 17[4] km/s
Age 2.72±0.78 Gyr
Other designations
γ Com, 15 Comae Berenices, BD+29° 2288, FK5 2999, GC 16964, HD 108381, HIP 60742, HR 4737, SAO 82313, PPM 101903[8]
Database references

Gamma Comae Berenices, Latinized from γ Comae Berenices, is a single,[9] orange-hued star in the southern constellation of Coma Berenices. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.36.[2] Based upon an annual parallax shift of 19.50 mas as seen from Earth, its distance can be estimated as around 167 light years from the Sun. The star is moving away from the Sun with a radial velocity of +3 km/s.[5]

This is an evolved K-type giant star with a stellar classification of K1 III Fe0.5.[3] The suffix notation indicates the star displays an overabundance of iron in its spectrum, it is most likely (91% chance) on the horizontal branch with an age of 2.7 billion years. If this is true, then it has an estimated 1.65 times the mass of the Sun and has expanded to nearly 12 times the Sun's radius. The star is radiating 58 times the Sun's luminosity from its enlarged photosphere at an effective temperature of around 4,652 K.[7] Gamma Comae Berenices appears as part of the Coma Star Cluster, although it is probably not actually a member of this cluster.[10]


  1. ^ a b c d e van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d Haupt, H. F.; Schroll, A. (1974), "Photoelektrische Photometrie von Shell-Sternen", Astronomy and Astrophysics Supplement Series, 15: 311, Bibcode:1974A&AS...15..311H. 
  3. ^ a b Keenan, Philip C; McNeil, Raymond C (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373. 
  4. ^ a b Hoffleit, D.; Warren, Jr., W. H., "HR 4737 database entry", The Bright Star Catalogue (5th Revised (Preliminary Version) ed.) 
  5. ^ a b Famaey, B.; et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430 (1): 165–186, arXiv:astro-ph/0409579Freely accessible, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272 
  6. ^ Hekker, S.; et al. (August 2006), "Precise radial velocities of giant stars. I. Stable stars", Astronomy and Astrophysics, 454 (3): 943–949, arXiv:astro-ph/0604502Freely accessible, Bibcode:2006A&A...454..943H, doi:10.1051/0004-6361:20064946 
  7. ^ a b Reffert, Sabine; et al. (2015), "Precise radial velocities of giant stars. VII. Occurrence rate of giant extrasolar planets as a function of mass and metallicity", Astronomy and Astrophysics, 574A (2): 116–129, arXiv:1412.4634Freely accessible, Bibcode:2015A&A...574A.116R, doi:10.1051/0004-6361/201322360. 
  8. ^ * gam Com -- Star in Cluster, database entry, SIMBAD. Accessed on line October 12, 2010.
  9. ^ 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:0806.2878Freely accessible, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x. 
  10. ^ Tonkin, Stephen F. (2007), Binocular astronomy, Springer, p. 124, ISBN 1-84628-308-6.