HD 187085 is a yellow–hued star in the southern constellation of Sagittarius. It is too faint to be visible to the naked eye, having an apparent visual magnitude of +7.225.[2] The star is located at a distance of approximately 1,010 light years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +18 km/s.[4]
This is an ordinary G-type main-sequence star with a stellar classification of G0V,[3] which means it is generating energy through core hydrogen fusion. It is younger than the Sun with an estimated age of 2.7 billion years and is spinning with a leisurely rotation period of around 21 days. The star is 27% larger and 19% more massive than the Sun.[2] It is radiating 2.3[1] times the luminosity of the Sun from its photosphere at an effective temperature of 6,117 K.[2]
In 2006, an extrasolar planet was announced orbiting HD 187085, with a minimum mass slightly below that of the planet Jupiter. It is orbiting the host star with a period of around 2.8 years.[6] The orbit overlaps the habitable zone of this star.[7] In 2009, the presence of an infrared excess was announced, suggesting a debris disk orbits the star.[8]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥0.836±0.011 MJ | 2.100±0.032 | 1,019.74+21.29 −22.58 |
0.251+0.221 −0.191 |
— | — |
See also
References
- ^ a b c d e f g h 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 f g Barbato, D.; et al. (August 2018), "Exploring the realm of scaled solar system analogues with HARPS", Astronomy & Astrophysics, 615: 21, arXiv:1804.08329, Bibcode:2018A&A...615A.175B, doi:10.1051/0004-6361/201832791, S2CID 119099721, A175.
- ^ a b Houk, Nancy (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 3, Ann Arbor, Michigan: Department of Astronomy, University of Michigan, Bibcode:1982mcts.book.....H.
- ^ a b c 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.
- ^ "HD 187085". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-09.
- ^ Jones, Hugh R. A.; et al. (2006), "High-eccentricity planets from the Anglo-Australian Planet Search", Monthly Notices of the Royal Astronomical Society, 369 (1): 249–256, arXiv:astro-ph/0603335, Bibcode:2006MNRAS.369..249J, doi:10.1111/j.1365-2966.2006.10298.x, S2CID 15452372.
- ^ Agnew, Matthew T.; et al. (November 2017), "Stable habitable zones of single Jovian planet systems", Monthly Notices of the Royal Astronomical Society, 471 (4): 4494–4507, arXiv:1706.05805, Bibcode:2017MNRAS.471.4494A, doi:10.1093/mnras/stx1449, S2CID 119227856.
- ^ Kóspál, Ágnes; et al. (August 2009), "On the Relationship Between Debris Disks and Planets", The Astrophysical Journal Letters, 700 (2): L73 – L77, arXiv:0907.0028, Bibcode:2009ApJ...700L..73K, doi:10.1088/0004-637X/700/2/L73, S2CID 16636256.
External links
- "Notes for star HD 187085". Extrasolar Planets Encyclopaedia. Archived from the original on July 2, 2007.
