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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]
Distance113.1 ± 0.2 ly
(34.69 ± 0.06 pc)
Absolute magnitude (MV)4.56[2]
Details
Mass1.032[5] M☉
Radius1.14±0.01[1] R☉
Luminosity1.253±0.003[1] L☉
Surface gravity (log g)4.39[5] cgs
Temperature5,722+11
−22[1] K
Metallicity [Fe/H]0.22±0.05[6] dex
Rotation31.7[6] days
Age7.6±2.4[2] Gyr
Other designations
BD–01°2431, HD 92788, HIP 52409, SAO 137743, LTT 3928, 2MASS J10424853-0211011[7]
Database references
SIMBADdata
Exoplanet Archivedata

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]

The HD 92788 planetary system[5]
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

  1. ^ 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.
  2. ^ 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. S2CID 119257644.
  3. ^ 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.
  4. ^ a b 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.
  5. ^ 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.
  6. ^ 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.
  7. ^ "HD 92788". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-04-02.
  8. ^ 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.
  9. ^ "hd_92788_b". Extrasolar Planets Encyclopaedia. Retrieved November 12, 2012.
  10. ^ 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.
  11. ^ 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.


source: https://en.wikipedia.org/wiki/HD_92788