HD 92788
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Sextans[1] |
| Right ascension | 10h 42m 48.52807s[2] |
| Declination | −02° 11′ 01.5221″[2] |
| Apparent magnitude (V) | 7.31[3] |
| Characteristics | |
| Spectral type | G6V[4] |
| B−V color index | 0.694±0.005[3] |
| Astrometry | |
| Radial velocity (Rv) | −4.455±0.0518[5] km/s |
| Proper motion (μ) | RA: −15.128±0.080[2] mas/yr Dec.: −223.230±0.061[2] mas/yr |
| Parallax (π) | 28.8281±0.0493 mas[2] |
| Distance | 113.1 ± 0.2 ly (34.69 ± 0.06 pc) |
| Absolute magnitude (MV) | 4.56[3] |
| Details | |
| Mass | 1.032[6] M☉ |
| Radius | 1.14±0.01[2] R☉ |
| Luminosity | 1.253±0.003[2] L☉ |
| Surface gravity (log g) | 4.39[6] cgs |
| Temperature | 5,722+11 −22[2] K |
| Metallicity [Fe/H] | 0.22±0.05[7] dex |
| Rotation | 31.7[7] days |
| Age | 7.6±2.4[3] Gyr |
| Other designations | |
| BD−01°2431, HD 92788, HIP 52409, SAO 137743, LTT 3928, 2MASS J10424853-0211011[8] | |
| 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.[3] 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.[5] Two planets have been found in orbit around the star.[6]
This is a G-type main-sequence star with a stellar classification of G6V.[4] It is estimated to be around eight billion years old and is spinning with a rotation period of 31.7 days.[7] The star has a similar mass to the Sun and is slightly larger in radius, with a high metallicity. It is radiating 1.25[2] times the luminosity of the Sun from its photosphere at an effective temperature of 5,722 K.[2]
Planetary system
[edit]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 with an orbital period of 0.89 years.[7] The star rotates at an inclination of 8+14
−8 degrees relative to Earth.[9] It is probable that this planet shares that inclination,[10][11] but direct measurements of the orbital inclinations via astrometry are inconsistent with the stellar rotational inclinaion.[12]
A second planetary companion was announced in 2019. Designated 'c', it orbiting with a period of around 27 years and a semimajor axis of 9.4 AU.[13]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination (°) |
Radius |
|---|---|---|---|---|---|---|
| b | 4.1+1.9 −0.5[12] MJ |
0.95±0.01[12] | 325.72±0.03[6] | 0.347±0.007[12] | 80±40[12] | — |
| c | 3.8+0.7 −0.6[12] MJ |
8.4±0.3[12] | 9,857±926[6] | 0.35+0.06 −0.05[12] |
100+40 −50[12] |
— |
References
[edit]- ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
- 1 2 3 4 5 6 7 8 9 10 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.
- 1 2 3 4 5 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.
- 1 2 Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
- 1 2 Soubiran, C.; et al. (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. S2CID 52952408.
- 1 2 3 4 5 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.
- 1 2 3 4 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. S2CID 6708869.
- ↑ "hd_92788_b". Extrasolar Planets 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. S2CID 38743202.
- 1 2 3 4 5 6 7 8 9 Van Zandt, Judah; Gilbert, Gregory J.; Petigura, Erik A.; Giacalone, Steven; Howard, Andrew W.; Handley, Luke B. (2026-04-02). "A Smooth Transition from Giant Planets to Brown Dwarfs from the Radial Occurrence Distribution". The Astronomical Journal. 171 (5): 267. doi:10.3847/1538-3881/ae5102. ISSN 0004-6256.
- ↑ 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. S2CID 91184450. A71.
External links
[edit]- "Notes for star HD 92788". Extrasolar Planets Encyclopaedia. Archived from the original on November 6, 2007. Retrieved 2008-08-30.
