The coalescence of white dwarfs and type I supernovae

Details The coalescence of white dwarfs and type I supernovae The coalescence of white dwarfs and type I supernovae

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...209..111m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 209, no. 1-2, Jan. 1989, p. 111-118. Research supported by the Loewengart Rese

Astronomy and Astrophysics

Astrophysics

40

Stellar Envelopes, Stellar Mass Accretion, Supernovae, White Dwarf Stars, Degenerate Matter, Giant Stars, Light Curve, Nuclear Fusion, Stellar Interiors

Scientific paper

Several aspects of the white dwarf coalescence scenario for type I supernovae are considered. Before coalescence, it is shown that synchronization of the binary white dwarf system is possible only if the tidal velocity field is turbulent, with a dissipation which can then reach 10 to the 38th erg/s at the moment of Roche-lobe overflow. Postcoalescence models involving a thick disk, rotating around a central white dwarf, which have the same total mass, angular momentum and energy as the initial system, are computed. Carbon ignition in rather low density material can be triggered during the coalescence process itself or later, by dissipation due to turbulence in the disk. The subsequent evolution of the object is very uncertain, even though its final explosion as a type I supernova remains a viable possibility.

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