Gamma Pavonis

Gamma Pavonis (γ Pav, γ Pavonis) is a star in the southern circumpolar constellation of Pavo. With an apparent visual magnitude of 4.22,[2] it is a fourth-magnitude star and thereby visible to the naked eye. From parallax observations with the Hipparcos satellite, the distance to this star has been estimated at 30.21 light-years (9.26 parsecs).[1]

Gamma Pavonis
Location of γ Pavonis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Pavo
Right ascension  21h 26m 26.60484s[1]
Declination −65° 21′ 58.3145″[1]
Apparent magnitude (V) 4.22[2]
Characteristics
Spectral type F9 V Fe-1.4 CH-0.7[3]
U−B color index −0.13[4]
B−V color index +0.48[4]
Variable type Suspected
Astrometry
Radial velocity (Rv)−29.9[5] km/s
Proper motion (μ) RA: +80.56[1] mas/yr
Dec.: +800.60[1] mas/yr
Parallax (π)107.97 ± 0.19[1] mas
Distance30.21 ± 0.05 ly
(9.26 ± 0.02 pc)
Absolute magnitude (MV)4.40[5]
Details
Mass1.21 ± 0.12[6] M☉
Radius1.15 ± 0.04[6] R☉
Luminosity1.52 ± 0.05[6] L☉
Surface gravity (log g)4.3[2] cgs
Temperature6,112[2] K
Metallicity [Fe/H]–0.80[2] dex
Rotational velocity (v sin i)1.0 ± 0.6[6] km/s
Age1.0[5] or 7.25[7] Gyr
Other designations
γ Pav, CD−65° 2751, FK5 805, GJ 827, HD 203608, HIP 105858, HR 8181, LHS 3674, LTT 8510, SAO 254999.
Database references
SIMBADdata

Compared to the Sun, this star has a 21% greater mass and a 15% larger radius. It is a brighter star with 152% of the Sun's luminosity,[6] which is it radiating from the outer envelope at an effective temperature of 6,112 K.[2] The stellar classification of F9 V[3] puts it in the class of F-type main sequence stars that generate energy through the nuclear fusion of hydrogen at the core. It is a metal-poor star, which means it has a low abundance of elements heavier than helium. Age estimates range from a low of a billion[5] years up to 7.25 billion years.[7] Gamma Pavonis is orbiting through the Milky Way at an unusually high peculiar velocity relative to nearby stars.

This star has rank 14 on TPF-C's top 100 target stars to search for a rocky planet in the Habitable Zone, approximately 1.2 AU, or a little beyond an Earth-like orbit.

References
  1. van Leeuwen, F. (November 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
  2. Jehin, E.; et al. (January 1999), "Abundance correlations in mildly metal-poor stars", Astronomy and Astrophysics, 341: 241–255, arXiv:astro-ph/9809405, Bibcode:1999A&A...341..241J
  3. Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637
  4. Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99), Bibcode:1966CoLPL...4...99J
  5. Holmberg, J.; Nordstrom, B.; Andersen, J. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics. 501 (3): 941–947. arXiv:0811.3982. Bibcode:2009A&A...501..941H. doi:10.1051/0004-6361/200811191.
  6. Bruntt, H.; et al. (July 2010), "Accurate fundamental parameters for 23 bright solar-type stars", Monthly Notices of the Royal Astronomical Society, 405 (3): 1907–1923, arXiv:1002.4268, Bibcode:2010MNRAS.405.1907B, doi:10.1111/j.1365-2966.2010.16575.x
  7. Mosser, B.; Deheuvels, S.; Michel, E.; Thévenin, F.; Dupret, M. A.; Samadi, R.; Barban, C.; Goupil, M. J. "HD 203608, a quiet asteroseismic target in the old galactic disk". Astronomy and Astrophysics. 488 (2): 635–642. arXiv:0804.3119. Bibcode:2008A&A...488..635M. doi:10.1051/0004-6361:200810011.
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