Accretion induced merger leading to core collapse supernovae in old stellar populations

Jessica Braudo, Ealeal Bear, Noam Soker

Published 2021-08-19Version 1

We examine a triple-star evolution that might lead to core collapse supernovae (CCSNe) in stellar populations that are too old to allow for single or binary evolution to form CCSNe, i.e., where the most massive stars that evolve off the main sequence have masses of ~4-5Mo. In the scenario we examine the most massive star in the triple system, of mass ~4-5Mo, transfers mass to an inner binary system at an orbital separation of ~100-1000Ro. The initial orbital separation of the inner binary is ~10-50Ro. The inner binary accretes most of the mass that the primary star loses and the two star expands and their mutual orbit contracts until merger. The merger product is a main sequence star of mass ~8-10o that later experience a CCSN explosion and leaves a NS remnant, bound or unbound to the white dwarf (WD) remnant of the primary star. We estimate the event rate of these WD-NS reverse evolution scenario be a fraction of ~5e-5 of CCSNe. We expect that in the coming decade sky surveys will detect 1-5 such events.