Neutrino Transport in Core Collapse Supernovae

Details Neutrino Transport in Core Collapse Supernovae Neutrino Transport in Core Collapse Supernovae

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004rpao.conf..224l&link_type=abstract

THE r-PROCESS The Astrophysical Origin of the Heavy Elements and Related Rare Isotope Accelerator Physics. Proceedings of the Fi

Physics

Nuclear Physics

Nuclear Theory

Scientific paper

A long lasting pursuit for accurate neutrino transport in core collapse supernovae appears to converge in spherically symmetric simulations. Under the restriction of spherical symmetry, the Boltzmann transport equation can be solved in extenso for neutrinos with individual energies and propagation directions. Comparisons between different numerical methods that solve or approximate the neutrino transport equation are summarized. Neutrino emission is the main channel for the release of the kinetic and thermal energy accrued during gravitational collapse. Recent supernova models with Boltzmann neutrino transport deliver detailed information about the corresponding neutrino luminosities and spectra as a function of time. The impact of the emitted neutrinos on accreted or ejected matter is estimated by the analysis of the equilibrium entropy and electron fraction at fixed neutrino background abundances. Final answers, however, will crucially depend on multidimensional effects, such as the convective turnover in the heating region or debated instabilities in the protoneutron star. What are the main technical difficulties to be encountered in multidimensional simulations and how are they currently approached?

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