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Motivated by recent discoveries of low-density super-Earths with shortorbital periods, we have investigated in-situ accretion of H-He atmospheres onrocky bodies embedded in dissipating warm disks, by simulating quasi-staticevolution of atmospheres that connect to the ambient disk. We have found thatthe atmospheric evolution has two distinctly different outcomes, depending onthe rocky body's mass: While the atmospheres on massive rocky bodies undergorunaway disk-gas accretion, those on light rocky bodies undergo significanterosion during disk dispersal. In the atmospheric erosion, the heat content ofthe rocky body that was previously neglected plays an important role. We havealso realized that the atmospheric mass is rather sensitive to disk temperaturein the mass range of interest in this study. Our theory is applied torecently-detected super-Earths orbiting Kepler-11 to examine the possibilitythat the planets are rock-dominated ones with relatively thick H-Heatmospheres. The application suggests that the in-situ formation of therelatively thick H-He atmospheres inferred by structure modeling is possibleonly under restricted conditions; namely, relatively slow disk dissipationand/or cool environments. This study demonstrates that low-density super-Earthsprovide important clues to understanding of planetary accretion and diskevolution.

In-situ Accretion of Hydrogen-Rich Atmospheres on Short-Period Super-Earths: Implications for the Kepler-11 Planets