Dependence of Deflagration Expansion on White Dwarf Mass

Details Dependence of Deflagration Expansion on White Dwarf Mass Dependence of Deflagration Expansion on White Dwarf Mass

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.1606w&link_type=abstract

American Astronomical Society, AAS Meeting #212, #16.06; Bulletin of the American Astronomical Society, Vol. 40, p.210

Astronomy and Astrophysics

Astronomy

Scientific paper

Type Ia supernovae are believed to be caused by thermonuclear detonations of white dwarf stars. The lead up to the possible detonation is still not well understood and there are several competing theories which involve a deflagration phase. In all cases, the subsonic nuclear burning by the deflagration causes the white dwarf to expand and the nucleosynthetic yield of any subsequent detonation is sensitive to the amount of expansion the white dwarf has undergone.
We explore the dependence of the expansion on the mass of the white dwarf at the beginning of the deflagration. We use the FLASH Code to carry out a series of 2-D axisymmetric simulations of the deflagration phase with white dwarfs of 1.36 to 1.40 solar masses. We compare the pulsational properties of the different white dwarfs and their estimated nucleosynthetic yields.

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