HD_76700

HD 76700

HD 76700

Star in the constellation Volans

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 197 light years from the Sun based on stellar parallax.[1] It is drifting further away with a radial velocity of +39 km/s.[2]

Quick Facts Observation data Epoch J2000.0 Equinox J2000.0, Constellation ...

Properties

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 the 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]

Planetary

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]

More information Companion (in order from star), Mass ...

References

  1. [1]
    Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. [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. S2CID 119257644.
  3. [3]
    Houk, Nancy; Cowley, A. P. (1979). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 1. Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
  4. [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. S2CID 54555839.
  5. [5]
    "HD 76700". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-11-07.
  6. [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. S2CID 10163020.
  7. [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. S2CID 54007702. 55.
  8. [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. S2CID 118438022.
  9. [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. S2CID 119067572.
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