Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...308..161h&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 308, Sept. 1, 1986, p. 161-175.
Astronomy and Astrophysics
Astrophysics
37
Binary Stars, Stellar Evolution, Supernovae, White Dwarf Stars, Accretion Disks, Angular Momentum, Dynamic Models, Equations Of State, Mass Transfer
Scientific paper
The authors examine the question of whether the merging white dwarfs result in a type I supernova. It has been argued that such a double white dwarf system forms from some intermediate-mass binary stars and will become a type I supernova as a result of merging. The numerical models presented here show that it is not probable that the less massive white dwarf is disrupted to form a heavy disk surrounding the more massive white dwarf. Instead, mass transfer from the less massive component will first form a common envelope. The common envelope will fill the outer critical Roche lobe, and mass outflow will begin from the outer Lagrangian point(s). Since this mass outflow is dynamically unstable, the two white dwarfs will merge in a dynamical time scale to form a single rapidly rotating white dwarf. If the initial mass of the double white dwarf is larger than 2.4 M_sun;, the merged object can become a type I supernova by igniting a carbon deflagration wave.
Eriguchi Yoshiharu
Hachisu Izumi
Nomaoto K.
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