The formation of compact objects in binary systems
Abstract
The observational evidence on compact objects in binary systems is summarized. Apart from the massive and the low-mass X-ray binaries, three binary radio pulsars are now known, PSR 1913 + 16, PSR 0656 + 64, and PSR 0820 + 02. The various ways in which compact objects can be formed in interacting binary systems are outlined. Massive interacting binary systems are, after the first phase of mass transfer expected to leave either: (1) Wolf-Rayet binaries, with a wide range of orbital periods, as a result of quasi-conservative mass transfer; or (2) systems with short orbital periods as remnants of highly nonconservative evolution (spiral-in during the first phase of mass transfer). From the fact that over 2/3 of all mass stars are members of binaries with P or = 10 yrs, it is argued that over 2/3 of all single pulsars are expected to have high runaway velocities, since they originate from disrupted post-spiral-in systems.
- Publication:
-
Astronomische Gesellschaft Abstract Series
- Pub Date:
- 1981
- Bibcode:
- 1981AGAb...51..121V
- Keywords:
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- Binary Stars;
- Mass Transfer;
- Pulsars;
- Stellar Evolution;
- Stellar Mass;
- Gravitational Collapse;
- Orbital Mechanics;
- Wolf-Rayet Stars;
- X Ray Binaries;
- Astrophysics