Efficient approximations of neutrino physics for three-dimensional simulations of stellar core collapse

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dc.creatorLiebendoerfer, M.
dc.creatorPen, U. -L.
dc.creatorThompson, C.
dc.date2006-09-24
dc.date.accessioned2026-07-07T10:23:40Z
dc.date.available2026-07-07T10:23:40Z
dc.descriptionNeutrino transport in spherically symmetric models of stellar core collapse and bounce has achieved a technically complete level, rewarded by the agreement among independent groups that a multi-dimensional treatment of the fluid-instabilities in the post-bounce phase is indispensable to model supernova explosions. While much effort is required to develop a reliable neutrino transport technique in axisymmetry, we explore neutrino physics approximations and parameterizations for an efficient three-dimensional simulation of the fluid-instabilities in the shock-heated matter that accumulates between the accretion shock and the protoneutron star. We demonstrate the reliability of a simple parameterization scheme in the collapse phase and extend our 3D magneto-hydrodynamical collapse simulations to a preliminary postbounce evolution. The growth of magnetic fields is investigated.
dc.description5 pages, 4 figures, in Proceedings of "Nuclei in the Cosmos IX, Geneva, Jun 25-30", associated movies are displayed at http://www.physik.unibas.ch/~liebend/display
dc.identifierhttps://arxiv.org/abs/astro-ph/0609651
dc.identifierhttp://arxiv.org/abs/astro-ph/0609651
dc.identifierPoSNIC-IX:132,2006
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175913
dc.subjectAstrophysics
dc.titleEfficient approximations of neutrino physics for three-dimensional simulations of stellar core collapse
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