HD 210277 b
| Discovery | |
|---|---|
| Discovered by | Marcy et al. |
| Discovery site | California and Carnegie Planet Search  USA |
| Discovery date | 9 Sept 1998 |
| Radial velocity | |
| Orbital characteristics | |
| 1.138 ± 0.066 AU (170,200,000 ± 9,900,000 km) | |
| Eccentricity | 0.476 ± 0.017 |
| 442.19 ± 0.50 d | |
| 2,450,104.3 ± 2.6 | |
| 119.1 ± 2.8 | |
| Semi-amplitude | 38.94 ± 0.75 |
| Star | HD 210277 |
HD 210277 b is an extrasolar planet orbiting the star HD 210277. It was discovered in September 1998 by the California and Carnegie Planet Search team using the highly successful radial velocity method. The planet is at least 24% more massive than Jupiter. The mean distance of the planet from the star is slightly more than Earth's distance from the Sun. However, the orbit is very eccentric, so at periastron this distance is almost halved, and at apastron it is as distant as Mars is from the Sun.[2]
In 2000, a group of scientists proposed, based on preliminary data from the Hipparcos astrometrical satellite, that the planet would have an inclination of 175.8° and a true mass of 18 times Jupiter making it a brown dwarf instead of a planet.[3] However these measurements were later proved useful only for upper limits of inclination.[4] If the planet orbits in the same plane as the claimed circumstellar disk, which seems a plausible assumption, it would have an inclination of 40° and an absolute mass of 2.2 times Jupiter,[5] however later observations failed to confirm the disk's existence.[6][7]
See also
[edit]References
[edit]- ^ 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.
- ^ Marcy, Geoffrey W.; et al. (1999). "Two New Planets in Eccentric Orbits". The Astrophysical Journal. 520 (1): 239–247. arXiv:astro-ph/9904275. Bibcode:1999ApJ...520..239M. doi:10.1086/307451. S2CID 16827678.
- ^ Han; Black, David C.; Gatewood, George (2001). "Preliminary Astrometric Masses for Proposed Extrasolar Planetary Companions". The Astrophysical Journal Letters. 548 (1): L57–L60. Bibcode:2001ApJ...548L..57H. doi:10.1086/318927. S2CID 120952927.
- ^ Pourbaix, D.; Arenou, F. (2001). "Screening the Hipparcos-based astrometric orbits of sub-stellar objects". Astronomy and Astrophysics. 372 (3): 935–944. arXiv:astro-ph/0104412. Bibcode:2001A&A...372..935P. doi:10.1051/0004-6361:20010597. S2CID 378792.
- ^ Trilling, D. E.; et al. (2000). "Circumstellar Dust Disks around Stars with Known Planetary Companions". The Astrophysical Journal. 529 (1): 499–505. Bibcode:2000ApJ...529..499T. doi:10.1086/308280. S2CID 121999545.
- ^ Beichman, C. A.; et al. (2005). "Planets and Infrared Excesses: Preliminary Results from a Spitzer MIPS Survey of Solar-Type Stars". The Astrophysical Journal. 622 (2): 1160–1170. arXiv:astro-ph/0412265. Bibcode:2005ApJ...622.1160B. doi:10.1086/428115. S2CID 6633656.
- ^ Bryden, G.; et al. (2009). "Planets and Debris Disks: Results from a Spitzer/MIPS Search for Infrared Excess". The Astrophysical Journal. 705 (2): 1226–1236. Bibcode:2009ApJ...705.1226B. doi:10.1088/0004-637X/705/2/1226.
External links
[edit]- "HD 210277". Exoplanets. Archived from the original on 2009-11-25. Retrieved 2008-10-29.
- The Planet Around HD 210277
- Location
- Simulation Exoplanets
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