HD 92788
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Sextans |
| Right ascension | 10h 42m 48.52807s[1] |
| Declination | −02° 11′ 01.5221″[1] |
| Apparent magnitude (V) | 7.31[2] |
| Characteristics | |
| Spectral type | G6V[3] |
| B−V color index | 0.694±0.005[2] |
| Astrometry | |
| Radial velocity (Rv) | −4.455±0.0518[4] km/s |
| Proper motion (μ) | RA: −15.128±0.080[1] mas/yr Dec.: −223.230±0.061[1] mas/yr |
| Parallax (π) | 28.8281 ± 0.0493 mas[1] |
| Distance | 113.1 ± 0.2 ly (34.69 ± 0.06 pc) |
| Absolute magnitude (MV) | 4.56[2] |
| Details | |
| Mass | 1.032[5] M☉ |
| Radius | 1.14±0.01[1] R☉ |
| Luminosity | 1.253±0.003[1] L☉ |
| Surface gravity (log g) | 4.39[5] cgs |
| Temperature | 5,722+11 −22[1] K |
| Metallicity [Fe/H] | 0.22±0.05[6] dex |
| Rotation | 31.7[6] days |
| Age | 7.6±2.4[2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HD 92788 is a star in the equatorial constellation of Sextans. It has a yellow hue but is too dim to be visible to the naked eye, having an apparent visual magnitude of 7.31.[2] The star is located at a distance of 113 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −4.5 km/s.[4] Two planets have been found in orbit around the star.[5]
This is a G-type main-sequence star with a stellar classification of G6V.[3] It is estimated to be around eight billion years old and is spinning with a rotation period of 31.7 days.[6] The star has a similar mass to the Sun and is slightly larger in radius, with a high metallicity. It is radiating 1.25[1] times the luminosity of the Sun from its photosphere at an effective temperature of 5,722 K.[1]
Planetary system
An extrasolar planet was discovered orbiting this star in 2001 by means of the radial velocity method. Designated component 'b', it is a Super-Jupiter or possibly a low-mass brown dwarf with an orbital period of 0.89 years.[6] The star rotates at an inclination of 8+14
−8 degrees relative to Earth.[8] It is probable that this planet shares that inclination.[9][10]
A low-mass brown dwarf companion was announced in 2019. Designated component 'c', it orbiting with a period of around 27 years and a semimajor axis of 9.4 AU.[11]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥3.78±0.18 MJ | 0.971±0.023 | 325.72±0.03 | 0.351±0.004 | — | — |
| c | ≥3.64±0.69 MJ | 9.43±0.63 | 9,857±926 | 0.18±0.08 | — | — |
See also
References
- ^ a b c d e f g h i j 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.
- ^ a b c d e 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.
- ^ a b Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
- ^ a b Soubiran, C.; Jasniewicz, G.; Chemin, L.; Zurbach, C.; Brouillet, N.; Panuzzo, P.; Sartoretti, P.; Katz, D.; Le Campion, J. -F.; Marchal, O.; Hestroffer, D.; Thévenin, F.; Crifo, F.; Udry, S.; Cropper, M.; Seabroke, G.; Viala, Y.; Benson, K.; Blomme, R.; Jean-Antoine, A.; Huckle, H.; Smith, M.; Baker, S. G.; Damerdji, Y.; Dolding, C.; Frémat, Y.; Gosset, E.; Guerrier, A.; Guy, L. P.; Haigron, R. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795.
{{cite journal}}: Unknown parameter|displayauthors=ignored (|display-authors=suggested) (help) - ^ a b c d Wittenmyer, Robert A.; et al. (April 2019). "Truly eccentric - I. Revisiting eight single-eccentric planetary systems". Monthly Notices of the Royal Astronomical Society. 484 (4): 5859–5867. arXiv:1901.08471. Bibcode:2019MNRAS.484.5859W. doi:10.1093/mnras/stz290.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ a b c d Fischer, Debra A.; et al. (2001). "Planetary Companions to HD 12661, HD 92788, and HD 38529 and Variations in Keplerian Residuals of Extrasolar Planets". The Astrophysical Journal. 551 (2): 1107–1118. Bibcode:2001ApJ...551.1107F. doi:10.1086/320224.
- ^ "HD 92788". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-04-02.
- ^ Simpson, E. K.; et al. (November 2010). "Rotation periods of exoplanet host stars". Monthly Notices of the Royal Astronomical Society. 408 (3): 1666–1679. arXiv:1006.4121. Bibcode:2010MNRAS.408.1666S. doi:10.1111/j.1365-2966.2010.17230.x.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ "hd_92788_b". Extrasolar Planet Encyclopaedia. Retrieved November 12, 2012.
- ^ Sanchis-Ojeda, Roberto; et al. (2012). "Starspots and spin-orbit alignment for Kepler cool host stars". Astronomische Nachrichten. 334 (1–2): 180–183. arXiv:1211.2002. Bibcode:2013AN....334..180S. doi:10.1002/asna.201211765.
- ^ Rickman, E. L.; et al. (May 2019). "The CORALIE survey for southern extrasolar planets. XVIII. Three new massive planets and two low-mass brown dwarfs at greater than 5 AU separation". Astronomy & Astrophysics. 625: 16. arXiv:1904.01573. Bibcode:2019A&A...625A..71R. doi:10.1051/0004-6361/201935356. A71.
External links
- "Notes for star HD 92788". The Extrasolar Planets Encyclopaedia. Retrieved 2008-08-30.
