The Evolution of Massive Close Binaries. V: Systems Containing Primaries with Masses between 10 Msun and 15 Msun
Abstract
The final state of the primaries of binary systems with initial massesM 1i=10M ⊙ to 15M ⊙ is derived from the mass of their C/O-cores. The possibility of a second stage of mass transfer towards the secondary is considered. It turns out that the critical mass for the bifurcation is about 14M ⊙: stars with larger masses in this range are the progenitors of neutron stars, while the lower mass stars are the ancestors of white dwarfs.
- Publication:
-
Astrophysics and Space Science
- Pub Date:
- August 1977
- DOI:
- 10.1007/BF00648520
- Bibcode:
- 1977Ap&SS..50...75D
- Keywords:
-
- Binary Stars;
- Mass Transfer;
- Stellar Evolution;
- Stellar Mass;
- Giant Stars;
- Neutron Stars;
- Nuclear Fusion;
- Stellar Models;
- White Dwarf Stars;
- Astrophysics