Evaluating Systematic Dependence of Type Ia Supernovae: The Influence of Progenitor Central Density

Details Evaluating Systematic Dependence of Type Ia Supernovae: The Influence of Progenitor Central Density Evaluating Systematic Dependence of Type Ia Supernovae: The Influence of Progenitor Central Density

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21733701k&link_type=abstract

American Astronomical Society, AAS Meeting #217, #337.01; Bulletin of the American Astronomical Society, Vol. 43, 2011

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We present a study of type Ia supernovae in the single-degenerate scenario, in which a white dwarf accretes mass from a companion star until it approaches the Chandrasekhar limiting mass and an explosion ensues. We investigate progenitor models with a range of central densities to study the influence of this parameter on explosion outcome. We present a suite of simulations from a well-controlled statistical study that allows us to quantify the effects of a variety of initial conditions. We present details of the models, including the mass and distribution of 56Ni, the radioactive decay of which powers the light curve. Our results indicate that progenitors with a higher central density produce less 56Ni and hence a dimmer event. We combine our results with those from previous studies by our collaboration to explore trends in explosion brightness that follow from properties related to the morphology and color of the host galaxy.
This work was supported by NASA under grant No. NNX09AD19G and utilized resources at the New York Center for Computational Sciences at Stony Brook University/Brookhaven National Laboratory, which is supported by the U.S. Department of Energy under Contract No. DE-AC02-98CH10886 and by the State of New York.

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