.jpg) | |
| Discovery | |
|---|---|
| Discovered by | C. Lovis et al.[1] |
| Discovery date | May 18, 2006 |
| Radial velocity | |
| Orbital characteristics | |
| 0.0764 ± 0.0017 AU (11,430,000 ± 250,000 km)[2] | |
| Eccentricity | 0.128±0.028[2] |
| 8.66897±0.00028 d[2] | |
| 2,453,496.8 ± 0.06 | |
| 340 ± 26 | |
| Semi-amplitude | 3.4±0.1 m/s[2] |
| Star | HD 69830 |
| Physical characteristics | |
| Mass | ≥10.1+0.38 −0.37 M🜨[2] |
| Temperature | ~804 K |
HD 69830 b is a Neptune-mass or super-Earth-mass exoplanet orbiting the star HD 69830. It is at least 10 times more massive than Earth. It also orbits very close to its parent star and takes 82/3 days to complete an orbit.
Based on theoretical modeling in the 2006 discovery paper, this is likely to be a rocky planet, not a gas giant.[1] However, other work has found that if it had formed as a gas giant, it would have stayed that way,[3] and it is now understood that planets this massive are rarely rocky.[4]
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.[5]
- ^ a b Cite error: The named reference
Lovis2006was invoked but never defined (see the help page). - ^ a b c d e Cite error: The named reference
Laliotis2023was invoked but never defined (see the help page). - ^ H. Lammer; et al. (2007). "The impact of nonthermal loss processes on planet masses from Neptunes to Jupiters" (PDF). Geophysical Research Abstracts. 9 (7850).
- ^ Chen, Jingjing; Kipping, David (2017). "Probabilistic Forecasting of the Masses and Radii of Other Worlds". The Astrophysical Journal. 834 (1): 17. arXiv:1603.08614. Bibcode:2017ApJ...834...17C. doi:10.3847/1538-4357/834/1/17. S2CID 119114880.
- ^ 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.