THE EFFECTS OF BINARY EVOLUTION ON THE DYNAMICS OF CORE COLLAPSE AND NEUTRON STAR KICKS

摘要: We systematically examine how the presence in a binary affects final core structure of massive star and its consequences for subsequent supernova explosion. Interactions with companion may change rate rotation, size helium core, strength carbon burning, iron mass. Stars initial masses larger than � 11 Mthat experience collapse will generally have smaller cores at point explosion if they lost their envelopes through interaction during or soon after hydrogen burning. below M� , on other hand, can end up metal close companion, since second dredge-up phase that reduces mass dramatically single stars does not occur once envelope is lost. find initially more systems range 8-11 Mare likely to undergo an electron-capture supernova, while same would as ONeMg white dwarfs. suggest (and possibly case relatively small cores) leads prompt fast rather very slow, delayed neutrino-driven this naturally produces neutron low-velocity kicks. This dichotomous distribution kicks, inferred previously, where binaries attain low kick velocities. illustrate such scenario using population synthesis simulations discuss implications. has also important minimum becomes star. For critical be high 10-12 it 6-8 .T hese depend treatment convection, amount convective overshooting, metal- licity star, lower amounts overshooting metallicity. Subject heading