Ott, Christian D. and Schnetter, Erik and Burrows, Adam and Livne, Eli and O'Connor, Evan and Löffler, Frank (2009) Computational models of stellar collapse and core-collapse supernovae. Journal of Physics: Conference Series, 180 . Art. No. 012022. ISSN 1742-6596. http://resolver.caltech.edu/CaltechAUTHORS:20100920-110700162
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Core-collapse supernovae are among Nature's most energetic events. They mark the end of massive star evolution and pollute the interstellar medium with the life-enabling ashes of thermonuclear burning. Despite their importance for the evolution of galaxies and life in the universe, the details of the core-collapse supernova explosion mechanism remain in the dark and pose a daunting computational challenge. We outline the multi-dimensional, multi-scale, and multi-physics nature of the core-collapse supernova problem and discuss computational strategies and requirements for its solution. Specifically, we highlight the axisymmetric (2D) radiation-MHD code VULCAN/2D and present results obtained from the first full-2D angle-dependent neutrino radiation-hydrodynamics simulations of the post-core-bounce supernova evolution. We then go on to discuss the new code Zelmani which is based on the open-source HPC Cactus framework and provides a scalable AMR approach for 3D fully general-relativistic modeling of stellar collapse, core-collapse supernovae and black hole formation on current and future massively-parallel HPC systems. We show Zelmani's scaling properties to more than 16,000 compute cores and discuss first 3D general-relativistic core-collapse results.
|Additional Information:||© 2009 IOP Publishing Ltd.|
|Classification Code:||PACS: 97.60.Bw; 98.62.Ai; 97.60.Lf; 97.10.Cv|
|Official Citation:||Christian D Ott et al 2009 J. Phys.: Conf. Ser. 180 012022 doi: 10.1088/1742-6596/180/1/012022|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Tony Diaz|
|Deposited On:||24 Sep 2010 22:06|
|Last Modified:||26 Dec 2012 12:26|
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