2005/10/14 by W. Schmidt, J. C. Niemeyer · 2 citations
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Gamma-ray bursts and supernovae #Neutrino Physics Research #astro-ph
paper · pdf · doi:10.1051/0004-6361:20054145
7 pages, 6 figures, accepted for publication in Astron. Astrophys.; PDF version with full resolution figures available from http://www.astro.uni-wuerzburg.de/~schmidt/Paper/StochIgnt_AA.pdf
arxiv created 2005/10/14 · openalex publication_date 2006/01/13 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/01
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 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 tends to be reduced for an ever increasing number of ignition events and, accordingly, more pronounced layering results.