Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.1851t&link_type=abstract
American Astronomical Society, HEAD meeting #9, #18.51; Bulletin of the American Astronomical Society, Vol. 38, p.390
Astronomy and Astrophysics
Astrophysics
Scientific paper
We present three-dimensional simulations of the deflagration phase of a Type Ia supernova which include post-flame neutronization, for the first time utilizing modern weak interaction rates, allowing us to quantify the degree of neutronization at various points in the deflagration. Many proposed mechanisms for Type Ia supernova explosions begin with a deflagration born near the center of a near Chandrasekhar mass C/O white dwarf. Large scale three-dimensional simulations of the progress of the deflagration through the star are being pursued in earnest in order to better understand the physical origins of the diversity observed in the SNIa population. The disparate range in the spatial scales between the flame front and the white dwarf prohibits direct simulation of the nuclear burning and thermal diffusion processes in a macroscopic simulation. A model flame and evolving hot ash are used to reproduce the nuclear energy release and composition changes in and behind the flame in order to enable accurate hydrodynamic simulation. Conversion of protons to neutrons in the hot, dense ash change the final composition of ejected material and provide a key observational diagnostic of the deflagration phase. In addition to the neutronization we determine the total energy released during the deflagration and the composition of the resulting material.
This work was supported by the U.S. Department of Energy under grant No. B523820 to the Center for Astrophysics Flashes and by the National Science Foundation under grant PHY 02-16783 to the Joint Institute for Nuclear Astrophysics and grant AST-0507456.
Asida Shimon M.
Brown Edward F.
Calder Alan C.
Jena Tridivesh
Lamb Don Q.
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