Statistics – Computation
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21543006k&link_type=abstract
American Astronomical Society, AAS Meeting #215, #430.06; Bulletin of the American Astronomical Society, Vol. 42, p.356
Statistics
Computation
Scientific paper
Recent observational studies of Type Ia supernovae (SNeIa) suggest correlations between the brightness of an event and properties of the host galaxy that may involve the age of the progenitor population. One way to influence the explosion systematically is through the ignition density, which is determined by both the mass of the white dwarf before the onset of accretion and the subsequent accretion history, and is therefore related to the age of the progenitor. We present the results of a suite of two-dimensional SNeIa simulations investigating how the central density of the progenitor white dwarf at flame ignition influences the production of Fe-group material, particularly the production of radioactive Ni-56 that powers the light curve. The simulation suite constitutes a theoretical population of events allowing a statistically well-controlled investigation into systematic trends (Townsley et al. 2009). The simulations indicate that with increased central density, more Fe-group material is produced but with less total Ni-56, which we attribute to a higher rate of neutronization occurring at higher density. Additionally, we compare our results with those of Roepke et al. (2006).
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.
Brown Edward F.
Calder Alan C.
Jackson Aaron P.
Krueger Brendan K.
Townsley Dean M.
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