Kepler-62 System Solar

The radii of the planets fall between 0. 54 and 1. 95 Earth radii. Of particular interest are the planets e and f, as they are the best candidates for solid planets falling into the habitable zone of their star. Their radii, 1. 61 and 1. 41 Earth radii respectively, put them in a radius range where they may be solid terrestrial planets. Their positions within the Kepler-62 system mean that they fall within Kepler-62’s habitable zone: the distance range where, for a given chemical composition (significant amounts of carbon dioxide for Kepler-62f, and a protective cloud cover for Kepler-62e), these two planets could have liquid water on their surfaces, perhaps completely covering them.
The masses of the planets could not be directly determined using either the radial velocity or the transit timing method; this failure leads to weak upper limits for the planets’ masses. For e and f, that upper limit amounts to 36 and 35 Earth masses, respectively; the real masses are expected to be significantly lower. Based on composition models, the real masses of the planets are probably likely to be 2. 1, 0. 1, 5. 5, 4. 8, and 2. 8 M⊕, respectively, taking into the uncertainty in composition and upper mass limits. The existence of an additional planet (at a distance of 0. 22 AU, between Kepler-62e and Kepler-62f) of the Kepler-62 system was predicted but not detected yet.