Double-core evolution and the formation of neutron star binaries with compact companions
Abstract
We present the results of a systematic exploration of an alternative evolutionary scenario to form double neutron star (DNS) binaries, first proposed by Brown (1995), which does not involve a neutron star passing through a common envelope. In this scenario, the initial binary components have very similar masses, and both components have left the main sequence before they evolve into contact; preferably the primary has already developed a CO core. We have performed population synthesis simulations to study the formation of DNS binaries via this channel and to predict the orbital properties and system velocities of such systems. We obtain a merger rate for DNSs in this channel in the range of 0.1-12Myr-1. These rates are still subject to substantial uncertainties such as the modelling of the contact phase.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- June 2006
- DOI:
- 10.1111/j.1365-2966.2006.10233.x
- arXiv:
- arXiv:astro-ph/0602510
- Bibcode:
- 2006MNRAS.368.1742D
- Keywords:
-
- binaries: general;
- stars: evolution;
- stars: neutron;
- Astrophysics
- E-Print:
- MNRAS, accepted