Stellar binaries that survive supernovae
Abstract
The number of binaries containing black holes (BH) or neutron stars (NS) depends critically on the fraction of binaries that survive supernova (SN) explosions. We searched for surviving star plus remnant binaries in a sample of 49 supernova remnants (SNR) containing 23 previously identified compact remnants and three highmass Xray binaries (HMXB), finding no new interacting or noninteracting binaries. The upper limits on any mainsequence stellar companion are typically ≲ 0.2 M_⊙ and are at worst ≲ 3 M_⊙. This implies that f < 0.1 of corecollapse SNRs contain a noninteracting binary, and f = 0.083 (0.032 < f < 0.17) contain an interacting binary at 90 per cent confidence. We also find that the transverse velocities of HMXBs are low, with a median of only 12 km s^{1} for field HMXBs, so surviving binaries will generally be found very close to the explosion centre. We compare the results to a `standard' StarTrack binary population synthesis (BPS) model, finding reasonable agreement with the observations. In particular, the BPS models predict that 6 per cent of initial binaries leave a star plus remnant binary, or 5 per cent of SNRs assuming an 84 per cent binary fraction.
 Publication:

Monthly Notices of the Royal Astronomical Society
 Pub Date:
 June 2019
 DOI:
 10.1093/mnras/stz717
 arXiv:
 arXiv:1810.08620
 Bibcode:
 2019MNRAS.485.5394K
 Keywords:

 stars: binaries;
 stars: massive;
 supernovae: general;
 Astrophysics  Solar and Stellar Astrophysics;
 Astrophysics  High Energy Astrophysical Phenomena
 EPrint:
 19 pages, 7 figures, 4 tables, submitted to MNRAS