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Core-Collapse Supernova Simulations including Neutrino Interactions from the Virial EOS

Published online by Cambridge University Press:  17 October 2017

Evan O’Connor ,
C. J. Horowitz ,
Zidu Lin  and
Sean Couch
Evan O’Connor
Affiliation:
Department of Astronomy and Oskar Klein Centre, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden email: evan.oconnor@astro.su.se NCSU, Department of Physics, Campus Code 8202, Raleigh, NC, 27695, USA
C. J. Horowitz
Affiliation:
Center for Exploration of Energy and Matter and Department of Physics, Indiana University, Bloomington, IN 47408, USA
Zidu Lin
Affiliation:
Center for Exploration of Energy and Matter and Department of Physics, Indiana University, Bloomington, IN 47408, USA
Sean Couch
Affiliation:
Department of Physics and Astronomy, MSU, East Lansing, MI 48824, USA Department of Computational Mathematics, Science, and Engineering, Michigan State University, East Lansing, MI 48824, USA National Superconducting Cyclotron Laboratory, MSU, East Lansing, MI 48824, USA Joint Institute for Nuclear Astrophysics, MSU, East Lansing, MI 48824, USA
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Abstract

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Core-collapse supernova explosions are driven by a central engine that converts a small fraction of the gravitational binding energy released during core collapse to outgoing kinetic energy. The suspected mode for this energy conversion is the neutrino mechanism, where a fraction of the neutrinos emitted from the newly formed protoneutron star are absorbed by and heat the matter behind the supernova shock. Accurate neutrino-matter interaction terms are crucial for simulating these explosions. In this proceedings for IAUS 331, SN 1987A, 30 years later, we explore several corrections to the neutrino-nucleon scattering opacity and demonstrate the effect on the dynamics of the core-collapse supernova central engine via two dimensional neutrino-radiation-hydrodynamics simulations. Our results reveal that the explosion properties are sensitive to corrections to the neutral-current scattering cross section at the 10-20% level, but only for densities at or above ~1012 g cm−3.

Keywords

(stars:) supernovae: generalstars: neutronmethods: numericalradiative transferneutrinoshydrodynamicsscattering
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S331: Supernova 1987A:30 years later - Cosmic Rays and Nuclei from Supernovae and their aftermaths , February 2017 , pp. 107 - 112
Copyright
Copyright © International Astronomical Union 2017 

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