HD 76700

HD 76700 is a star in the southern constellation of Volans. It is yellow in hue and is too faint to be visible to the naked eye, having an apparent visual magnitude of 8.16.[2] This object is located at a distance of 199 light years from the Sun based on stellar parallax.[1] It is drifting further away with a radial velocity of +39 km/s.[2]

HD 76700
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Volans
Right ascension  08h 53m 55.5159s[1]
Declination −66° 48′ 03.5743″[1]
Apparent magnitude (V) 8.16[2]
Characteristics
Spectral type G6V[3]
B−V color index 0.745±0.010[2]
Astrometry
Radial velocity (Rv)+38.90±1.46[2] km/s
Proper motion (μ) RA: −282.828±0.056[1] mas/yr
Dec.: +120.362±0.056[1] mas/yr
Parallax (π)16.3960 ± 0.0314[1] mas
Distance198.9 ± 0.4 ly
(61.0 ± 0.1 pc)
Absolute magnitude (MV)4.26[2]
Details[4]
Mass1.10±0.02 M☉
Radius1.34±0.03 R☉
Luminosity1.69±0.01 L☉
Surface gravity (log g)4.22±0.03 cgs
Temperature5,694±44 K
Metallicity [Fe/H]+0.31±0.02[2] dex
Age6.9±0.8 Gyr
Other designations
CD−66°656, HD 76700, HIP 43686, SAO 250370, LTT 3291, NLTT 20555, 2MASS J08535550-6648034[5]
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

This object is a G-type main-sequence star with a stellar classification of G6V,[3] which indicates it is generating energy through core hydrogen fusion. It is a metal-enriched star, showing a much higher metallicity than the Sun.[6] This may be explained by prior accretion of refractory-rich planetary bodies into the stellar atmosphere.[7] The mass of HD 76700 is very similar to (1.1 times) that of our Sun, but it is cooler and brighter (with an effective temperature of 5,694 K and luminosity of 1.69 Suns) and thus much older—around 6.9 billion years old.[4]

HD 76700 is orbited by a giant planet that was discovered in 2003 via the radial velocity method.[6] Designated HD 76700 b, this planet is orbiting very close to the star with a period of just four days.[8]

The HD 76700 planetary system[8]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥ 0.23 MJ 0.0511±0.0030[9] 3.97101±0.00020 0.0616+0.0426
−0.0587		 — 0.99 RJ

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015.
  3. Houk, Nancy; Cowley, A. P. (1979). "Michigan catalogue of two-dimensional spectral types for the HD stars". 1. Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H. Cite journal requires |journal= (help)
  4. Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy & Astrophysics. 575 (A18): 17. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951.
  5. "HD 76700". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-11-07.
  6. Tinney, C. G.; et al. (2003). "Four New Planets Orbiting Metal-enriched Stars". The Astrophysical Journal. 587 (1): 423–428. arXiv:astro-ph/0207128. Bibcode:2003ApJ...587..423T. doi:10.1086/368068.
  7. Schuler, Simon C.; et al. (May 2011). "Abundances of Stars with Planets: Trends with Condensation Temperature". The Astrophysical Journal. 732 (1): 15. arXiv:1103.0757. Bibcode:2011ApJ...732...55S. doi:10.1088/0004-637X/732/1/55. 55.
  8. Wang, Ji; Ford, Eric B. (December 2011). "On the eccentricity distribution of short-period single-planet systems". Monthly Notices of the Royal Astronomical Society. 418 (3): 1822–1833. arXiv:1108.1811. Bibcode:2011MNRAS.418.1822W. doi:10.1111/j.1365-2966.2011.19600.x.
  9. Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701.

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