Evolution of binary compact objects which merge
Feb, 199832 pages
Published in:
- Astrophys.J. 506 (1998) 780-789
e-Print:
- astro-ph/9802084 [astro-ph]
DOI:
Report number:
- SUNY-NTG-98-4
Citations per year
Abstract: (arXiv)
Beginning from massive binaries in the Galaxy we evolve black-hole, neutron-star binaries and binary neutron stars, such as the Hulse-Taylor system PSR 1913+16. The new point in our evolution is a quantitative calculation of the accretion of matter by a neutron star in common envelope evolution which sends it into a black hole. We calculate the mass of the latter to be \sim 2.4\msun. Our chief conclusion is that the production rate for black-hole, neutron-star binaries (in which the neutron star is unrecycled) is per year per Galaxy, an order of magnitude greater than that of neutron star binaries. Not only should this result in a factor of 10 more mergings for gravitational wave detectors like LIGO, but the signal should be larger. We give some discussion of why black-hole, neutron-star binaries have not been observed, but conclude that they should be actively searched for.References(19)
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