Evolution of Massive Close Binaries. IV: Evolution of a 10 Msun+8 Msun System into a System with a White Dwarf Component
Abstract
The evolution of a binary system with components of 10M ⊙ and 8M ⊙ is computed through a case B of mass exchange. It is found that after the end of core helium burning, a second stage of mass transfer from the primary occurs. Carbon ignition is prohibited by the large neutrino losses in the degenerated core. The primary remnant, a 1.12M ⊙ star, ends as a white dwarf. A comparison with the 10M ⊙ single evolution is made.
- Publication:
-
Astrophysics and Space Science
- Pub Date:
- August 1976
- DOI:
- 10.1007/BF00640553
- Bibcode:
- 1976Ap&SS..43...35D
- Keywords:
-
- Binary Stars;
- Stellar Evolution;
- Stellar Mass;
- White Dwarf Stars;
- Carbon;
- Computerized Simulation;
- Helium;
- Mass Transfer;
- Neutrinos;
- Nuclear Fusion;
- Astrophysics