HD 69830 b
| Discovery | |
|---|---|
| Discovered by | C. Lovis et al. |
| Discovery date | May 18, 2006 |
| Radial velocity | |
| Orbital characteristics | |
| 0.0764 ± 0.0017 AU (11,430,000 ± 250,000 km) | |
| Eccentricity | 0.128±0.028 |
| 8.66897±0.00028 d | |
| 2,453,496.8 ± 0.06 | |
| 340 ± 26 | |
| Semi-amplitude | 3.4±0.1 m/s |
| Star | HD 69830 |
| Physical characteristics | |
| Mass | ≥10.1+0.38 −0.37 M🜨 |
| 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. However, other work has found that if it had formed as a gas giant, it would have stayed that way, and it is now understood that planets this massive are rarely rocky.
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.