Origin of the binary pulsar PSR 1913 + 16
We suggest that the progenitor of the binary pulsar PSR 1913 + 16 could have been a cataclysmic variable (CV)-binary or an evolved massive X-ray binary. In both cases a range of satisfactory initial binary periods and masses can be found if one postulates that a small kick (approximately 200 km/s) is imparted to the remnant pulsar by a slightly asymmetric supernova explosion. In the second case such an asymmetric explosion is not absolutely required. In the first (CV)- scenario the companion of the pulsar is a temporarily undersized lower main- sequence star, stripped of its envelope by the explosion. In this case the apsidal motion period of the PSR 1913 + 16 system is predicted to be a few months; upon reexpansion of the companion, such a system may become a low-mass X- ray binary of a type similar to Sco X-1. The second scenario implies that the companion is a collapsed star and the system has only a small general relativistic apsidal motion. (orig.)
- Research Organization:
- Institute for Advanced Study, Princeton, N.J. (USA)
- NSA Number:
- NSA-33-010005
- OSTI ID:
- 4123936
- Journal Information:
- Astron. Astrophys., v. 39, no. 1, pp. 61-67, Journal Name: Astron. Astrophys., v. 39, no. 1, pp. 61-67; ISSN AAEJA
- Country of Publication:
- Germany
- Language:
- English
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