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C. Diehl

Research: Simulations of planets around post-common envelope binary systems with the FLASH code

By now, several planets have been detected around binary star systems via the eclipse timing variation method. Among them are planets in post-common envelope binaries where one or both of the stellar components evolved past the Main Sequence to White Dwarfs and during this evolution shared a common gaseous envelope with their stellar companion. Making use of FLASH, an adaptive mesh refinement simulation code for multiple physical demands, we simulate planets around close binary stars during and after the common envelope phase. The change in the gravitational potential of the binary combined with momentum transfer between planets and expelled gas can have significant effects on the dynamics of these planets. On the one hand, possible outcomes of the stellar evolution include the expulsion or destruction of planets. On the other hand, a circumbinary disk could be formed and lead to gas accretion onto existing planets or even the formation of new (second generation) planets. Exemplary system: NN Serpentis