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The close binary system NN Serpentis must have gone through a common envelopephase before the formation of its white dwarf. During this phase, a substantialamount of mass was lost from the envelope. The recently detected orbits ofcircumbinary planets are likely inconsistent with planet formation before themass loss.We explore whether new planets may have formed from the ejecta of thecommon envelope and derive the expected planetary mass as a function ofradius.We employed the Kashi & Soker model to estimate the amount of mass thatis retained during the ejection event and inferred the properties of theresulting disk from the conservation of mass and angular momentum. Theresulting planetary masses were estimated from models with and withoutradiative feedback. We show that the observed planetary masses can bereproduced for appropriate model parameters. Photoheating can stabilize thedisks in the interior, potentially explaining the observed planetary orbits onscales of a few AU. We compare the expected mass scale of planets for 11additional systems with observational results and find hints of twopopulations, one consistent with planet formation from the ejecta of commonenvelopes and the other a separate population that may have formed earlier. Theformation of the observed planets from the ejecta of common envelopes seemsfeasible. The model proposed here can be tested through refined observations ofadditional post-common envelope systems. While it appears observationallychallenging to distinguish between the accretion on pre-existing planets andtheir growth from new fragments, it may be possible to further constrain theproperties of the protoplanetary disk through additional observations ofcurrent planetary candidates and post-common envelope binary systems.

Planet formation from the ejecta of common envelopes