| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Volans |
| Right ascension | 08 53 55.5161 |
| Declination | −66° 48′ 03.576″ |
| Apparent magnitude (V) | 8.16 |
| Characteristics | |
| Spectral type | G6V |
| B−V color index | 0.745±0.010 |
| Astrometry | |
| Radial velocity (Rv) | +38.90±1.46 km/s |
| Proper motion (μ) | RA: −282.929(47) mas/yr Dec.: 120.479(43) mas/yr |
| Parallax (π) | 16.5671 ± 0.0387 mas |
| Distance | 196.9 ± 0.5 ly (60.4 ± 0.1 pc) |
| Absolute magnitude (MV) | 4.26 |
| Details | |
| Mass | 1.10±0.02 M☉ |
| Radius | 1.34±0.03 R☉ |
| Luminosity | 1.69±0.01 L☉ |
| Surface gravity (log g) | 4.22±0.03 cgs |
| Temperature | 5,694±44 K |
| Metallicity ※ | +0.31±0.02 dex |
| Age | 6.9±0.8 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
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. This object is located at a distance of 197 light years from the Sun based on stellar parallax. It is drifting further away with a radial velocity of +39 km/s.
Properties※
This object is a G-type main-sequence star with a stellar classification of G6V, which indicates it is generating energy through core hydrogen fusion. It is a metal-enriched star, showing much higher metallicity than the Sun. This may be explained by, prior accretion of refractory-rich planetary bodies into the stellar atmosphere. 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.
Planetary※
HD 76700 is orbited by a giant planet that was discovered in 2003 via the radial velocity method. Designated HD 76700 b, this planet is orbiting very close to the star with a period of just four days.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥ 0.23 MJ | 0.0511±0.0030 | 3.97101±0.00020 | 0.0616+0.0426 −0.0587 |
— | 0.99 RJ |
References※
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ "HD 76700". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-11-07.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
