HD 69830 b
.jpg) | |
| Discovery | |
|---|---|
| Discovered by | C. Lovis et al.[1] |
| Discovery date | May 18, 2006 |
| Radial velocity | |
| Orbital characteristics | |
| 0.0785 AU (11,740,000 km) | |
| Eccentricity | 0.1 ± 0.04 |
| 8.667 ± 0.003 d | |
| 2,453,496.8 ± 0.06 | |
| 340 ± 26 | |
| Semi-amplitude | 3.51 ± 0.15 |
| Star | HD 69830 |
| Physical characteristics | |
| Temperature | ~804 K |
HD 69830 b is a Neptune-mass or super-Earth-mass exoplanet orbiting the star HD 69830. It is 10 times more massive than Earth. It also orbits very close to its parent star and takes 82/3 days to complete an orbit.
This is likely to be a rocky planet, not a gas giant.[1] If it had formed as a gas giant, it would have stayed that way.[2]
If HD 69830 b is a terrestrial planet, models predict that tidal heating would produce a heat flux at the surface of about 55 W/m2. This is 20 times that of Io.[3]
References
- ^ a b Lovis, Christophe; et al. (2006). "An extrasolar planetary system with three Neptune-mass planets" (PDF). Nature. 441 (7091): 305–309. arXiv:astro-ph/0703024. Bibcode:2006Natur.441..305L. doi:10.1038/nature04828. PMID 16710412. S2CID 4343578.
- ^ H. Lammer; et al. (2007). "The impact of nonthermal loss processes on planet masses from Neptunes to Jupiters" (PDF). Geophysical Research Abstracts. 9 (7850).
- ^ Jackson, Brian; Richard Greenberg; Rory Barnes (2008). "Tidal Heating of Extra-Solar Planets". Astrophysical Journal. 681 (2): 1631. arXiv:0803.0026. Bibcode:2008ApJ...681.1631J. doi:10.1086/587641. S2CID 42315630.
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