"As many young massive stars are found in close binaries, many core-collapse supernova progenitors are expected to experience binary interaction before exploding. We employ simple analytical estimates as well as more sophisticated population synthesis simulations to quantify the expected fraction of binary interactions, focusing on hydrogen-rich supernovae progenitors. In all our simulations, each for different assumptions, we find that around 1/2 to 1/3 of all type II supernovae progenitors experience some kind of mass exchange with a companion, like mass accretion, common envelope evolution and/or merging.
This variety of the possible binary evolutionary channels may help explain the diversity in the observed properties of SN II and may account for a portion of some peculiar SN II subclasses. This is because binary interaction influences the structure of the progenitor from the one expected from single-stellar evolution and is also a way to eject circumstellar material in the vicinity of the progenitor, needed to give rise to features of interaction during the SN events.
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