HD 69830 b

HD 69830 b
Discovery
Discovered byC. Lovis et al.[1]
Discovery dateMay 18, 2006
Radial velocity
Orbital characteristics
0.0764 ± 0.0017 AU (11,430,000 ± 250,000 km)[2]
Eccentricity0.128±0.028[2]
8.66897±0.00028 d[2]
2,453,496.8 ± 0.06
340 ± 26
Semi-amplitude3.4±0.1 m/s[2]
StarHD 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]

  1. ^ a b Cite error: The named reference Lovis2006 was invoked but never defined (see the help page).
  2. ^ a b c d e Cite error: The named reference Laliotis2023 was invoked but never defined (see the help page).
  3. ^ H. Lammer; et al. (2007). "The impact of nonthermal loss processes on planet masses from Neptunes to Jupiters" (PDF). Geophysical Research Abstracts. 9 (7850).
  4. ^ 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.
  5. ^ 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.