Thermonuclear Supernovae: Simulations of the Deflagration Stage and Their Implications
Vadim N. Gamezo,1*
Alexei M. Khokhlov,1
Elaine S. Oran,1
Almadena Y. Chtchelkanova,3
Robert O. Rosenberg2
Large-scale, three-dimensional numerical simulations of the
deflagration stage of a thermonuclear supernova explosion show the
formation and evolution of a highly convoluted turbulent flame in the
gravitational field of an expanding carbon-oxygen white dwarf. The
flame dynamics are dominated by the gravity-induced Rayleigh-Taylor
instability that controls the burning rate. The thermonuclear
deflagration releases enough energy to produce a healthy explosion. The
turbulent flame, however, leaves large amounts of unburned and
partially burned material near the star center, whereas observations
that imply these materials are present only in outer layers. This
disagreement could be resolved if the deflagration triggers a
detonation.
1 Laboratory for Computational Physics and
Fluid Dynamics, Naval Research Laboratory (NRL),
2 Center for Computational Science, NRL, Washington,
DC 20375, USA.
3 Strategic Analysis Incorporated,
Arlington, VA 22201, USA.
*
To whom correspondence should be addressed. E-mail:
gamezo{at}lcp.nrl.navy.mil
