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Planets that form early enough to be embedded in the circumstellar gas diskaccumulate thick atmospheres of nebular gas. Models of these atmospheres needto specify the surface luminosity (i.e. energy loss rate) of the planet. Thisluminosity is usually associated with a continuous inflow of solid bodies,where the gravitational energy released from these bodies is the source ofenergy. However, if these bodies release energy in the atmosphere instead of atthe surface, this assumption might not be justified. Our aim is to explore theinteractions of infalling planetesimals with primordial atmospheres at anembedded phase of evolution. We investigate effects of atmospheric interactionon the planetesimals (mass loss) and the atmosphere (heating/cooling). We usedatmospheric parameters from a snapshot of time-dependent evolution simulationsfor embedded atmospheres and simulated purely radial, infall events ofsiliceous planetesimals in a 1D, explicit code. We implemented energy transferbetween friction, radiation transfer by the atmosphere and the body and thermalablation; this gives us the possibility to examine the effects on theplanetesimals and the atmosphere. We find that a significant amount ofgravitational energy is indeed dissipated into the atmosphere, especially forlarger planetary cores, which consequently cannot contribute to the atmosphericplanetary luminosity. Furthermore, we examine that planetesimal infall eventsfor cores, $M_\mathrm{C} > 2$M$_{\oplus}$, which actually result in a localcooling of the atmosphere; this is totally in contradiction with the classicalmodel.

Interaction of infalling solid bodies with primordial atmospheres of disk-embedded planets