Because Kepler-10 is one of the brighter stars being targeted by Kepler, scientists were able to detect high frequency variations in the star's brightness generated by stellar oscillations, or starquakes. This analysis allowed scientists to pin down Kepler-10b's properties. There is a clear sign...
Because of the multiple bodies it made measuring properties such as mass and orbital period easier to discern. In January of 2011 the first rocky planet, Kepler-10b, was not only discovered but also found to be 1.4 Earth masses. Even smaller ones were eventually found....
Validation of Planet Kepler-11g The outer planetary candidate is well-separated from the inner five in orbital period, and its dynamical interactions are not manifested in the data presently available. Thus, we only have a weak upper bound on its mass, and unlike the other five candidates, ...
When an extrasolar planet passes in front of (transits) its star, its radius can be measured from the decrease in starlight and its orbital period from the time between transits. Multiple planets transiting the same star reveal much more: period ratios d
The orbital migration has been more important for sub-Neptunes than for super-Earths, suggesting a partial ex situ formation of the former and an origin of the radius valley caused in part by distinct formation pathways. However, the model comparisons also show that ...
Two USP planets, namely Kepler-10b and Kepler-78b, show non-negligible nightside emission. This questions the scenario of magma-ocean worlds with inefficient heat redistribution to the nightside for both planets. Due to the youth of the Kepler-78 system and the small planetary orbital separation,...
We also found 3 cases of candidates which showed some changes of the orbital period. Based on our results we can see that orbital period changes are not caused by comet-like tail disintegration processes, but rather by possible massive outer companions. ( 2014 WILEY-VCH Verlag GmbH & Co. ...