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Formation of planets in the Neptune size range with low-mass, but voluminous,H_2/He gaseous envelopes is modeled by detailed numerical simulations accordingto the core-nucleated accretion scenario. Formation locations ranging from 0.5to 4 AU from a star of 1 solar mass are considered. The final planets haveheavy-element cores of 2.2--2.5 Earth masses and envelopes in the range0.037--0.16 Earth masses. After the formation process, which lasts 2 Myr orless, the planets evolve at constant mass up to an age of several Gyr. Forassumed equilibrium temperatures of 250, 500, and 1000 K, their calculatedfinal radii are compared with those observed by the Kepler spacecraft. For theparticular case of Kepler-11 f, we address the question whether it could haveformed in situ or whether migration from a formation location farther out inthe disk is required.

Accretion and Evolution of ~2.5 Earth-mass Planets with Voluminous H/He Envelopes