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Issue A&A
Volume 446, Number 2, February I 2006
Page(s) 627 - 633
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20054145

A&A 446, 627-633 (2006)
DOI: 10.1051/0004-6361:20054145

Thermonuclear supernova simulations with stochastic ignition

W. Schmidt and J. C. Niemeyer

Lehrstuhl für Astronomie, Institut für Theoretische Physik und Astrophysik, Universität Würzburg, Am Hubland, 97074 Würzburg, Germany
    e-mail: schmidt@astro.uni-wuerzburg.de

(Received 15 July 2005 / Accepted 11 October 2005)

Abstract
We apply an ad hoc model for dynamical ignition in three-dimensional numerical simulations of thermonuclear supernovae assuming pure deflagrations. The model makes use of the statistical description of temperature fluctuations in the pre-supernova core proposed by Wunsch & Woosley (2004, ApJ, 616, 1102). Randomness in time is implemented by means of a Poisson process. We are able to vary the explosion energy and nucleosynthesis depending on the free parameter of the model which controls the rapidity of the ignition process. However, beyond a certain threshold, the strength of the explosion saturates and the outcome appears to be robust with respect to the number of ignitions. In the most energetic explosions, we find about $0.75~M_{\odot}$ of iron group elements. Other than in simulations with simultaneous multi-spot ignition, the amount of unburned carbon and oxygen at radial velocities of a few $10^{3}\,{\rm km\,s^{-1}}$ tends to be reduced for an ever increasing number of ignition events and, accordingly, more pronounced layering results.


Key words: stars: supernovae: general -- methods: numerical -- stars: evolution -- stars: interiors





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