Nucleosynthesis in Surface Detonation Type Ia Supernovae

Details Nucleosynthesis in Surface Detonation Type Ia Supernovae Nucleosynthesis in Surface Detonation Type Ia Supernovae

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1016..472s&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: The 10th International Symposium on Origin of Matter and Evolution of Galaxies: From

Statistics

Computation

1

Cosmic Ray Nucleosynthesis, Supernova Remnants, Thermodynamics

Scientific paper

A common method for calculating nucleosynthetic yields for Type Ia supernovae (SNe Ia) is the post-processing of a large number of passively advected tracer particles with a nuclear reaction network. In this paper we present a novel and more computationally efficient method for calculating nucleosynthetic yields for material burned to nuclear statistical equilibrium (NSE). The method exploits a tight correlation that exists between the final entropy and neutron excess for material processed by a detonation. We generate a table of freeze out abundances by integrating a 443 nuclide nuclear reaction network along synthetic thermodynamic trajectories at a fixed entropy and neutron excess. Final yields are calculated by first interpolating in the table and then decaying short lived radionuclides back to stability.
We apply this method to obtain Fe-peak yields for a suite of 2D axisymmetric SNe Ia simulations in the framework of the gravitationally confined detonation (GCD) explosion mechanism developed at the Flash Center. Our models produce 56Ni masses that are comparable to observed high luminosity SNe Ia and have a reasonable isotopic composition of other Fe-peak elements.

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