Three-dimensional Hydrodynamical Simulations of Stellar Collision. II. White Dwarfs
Abstract
Three-dimensional numerical simulations are presented for collisions between white dwarfs, using a smooth-particle hydrodynamics code with 5000 particles. The code allows for radiation and degenerate pressure and uses a reduced nuclear network which models the large release of nuclear energy. Two different collision models are considered over a range of impact parameters: between two 0.6 solar-mass C-O white dwarfs and between 0.9 solar-mass and 0.7 solar-mass C-O white dwarfs. In nearly head-on collisions, a very substantial fraction of the mass is lost as a result of a large release of nuclear energy. In grazing collisions, the fraction of mass lost is close to that produced in collisions between main-sequence stars. The quantity of processed elements ejected into the ISM by these collisions does not significantly affect the chemical evolution of the Galaxy.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- July 1989
- DOI:
- 10.1086/167656
- Bibcode:
- 1989ApJ...342..986B
- Keywords:
-
- Collisions;
- Computational Astrophysics;
- Hydrodynamics;
- Stellar Motions;
- Three Dimensional Models;
- White Dwarf Stars;
- Chemical Evolution;
- Digital Simulation;
- Main Sequence Stars;
- Milky Way Galaxy;
- Nuclear Energy;
- Stellar Interiors;
- Stellar Mass Ejection;
- Astrophysics;
- HYDRODYNAMICS;
- STARS: INTERIORS;
- STARS: MASS LOSS;
- STARS: WHITE DWARFS