Volume 413, Number 1, January I 2004
|Page(s)||257 - 272|
|Section||Stellar structure and evolution|
|Published online||17 December 2003|
Smoothed Particle Hydrodynamics simulations of merging white dwarfs*
Institute for Space Studies of Catalonia, c/Gran Capitá 2–4, Edif. Nexus 104, 08034 Barcelona, Spain
2 Departament de Física Aplicada, Escola Politécnica Superior de Castelldefels, Universitat Politécnica de Catalunya, Avda. del Canal Olímpic s/n, 08860 Castelldefels, Spain
3 Institut de Ciéncies de l'Espai, C.S.I.C.
Corresponding author: E. García–Berro, email@example.com
Accepted: 4 September 2003
We present the results of three-dimensional Smoothed Particle Hydrodynamics (SPH) calculations of the process of coalescence of white dwarfs. We follow in detail the initial phase of the merging for several masses of the primary and the secondary of the binary system. Special attention has been paid to the issue of whether or not thermonuclear runaway occurs during the process of merging. We find that although relatively high temperatures are attained during the most violent phase of the merging process, the thermonuclear flash is rapidly quenched. The total mass lost by the system is also relatively small (of the order of 0.5% at most) except for the most massive primaries for which it is still small (~). Consequently, a heavy accretion disk around the primary is formed. We also discuss the subsequent evolution of the resulting system and the possible astrophysical scenarios of interest.
Key words: stars: white dwarfs / stars: interiors / stars: binaries: close / hydrodynamics / methods: numerical / accretion, accretion disks
© ESO, 2004
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