Coupling Neutrino Oscillations and Simulations of Core-Collapse Supernovae. (arXiv:1910.04172v1 [astro-ph.HE])

Coupling Neutrino Oscillations and Simulations of Core-Collapse Supernovae. (arXiv:1910.04172v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Stapleford_C/0/1/0/all/0/1">Charles J. Stapleford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frohlich_C/0/1/0/all/0/1">Carla Fr&#xf6;hlich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kneller_J/0/1/0/all/0/1">James P. Kneller</a>

At the present time even the most sophisticated, multi-dimensional
simulations of core-collapse supernovae do not (self-consistently) include
neutrino flavor transformation. This physics is missing despite the importance
of neutrinos in the core-collapse explosion paradigm. Because of this
dependence, any flavor transformation that occurs in the region between the
proto-neutron star and the shock could result in major effects upon the
dynamics of the explosion. We present the first hydrodynamic core-collapse
supernova simulation which simultaneously includes flavor transformation of the
free-streaming neutrinos in the neutrino transport. These oscillation
calculations are dynamically updated and evolve self-consistently alongside the
hydrodynamics. Using a $M=20;{rm M_{odot}}$ progenitor, we find that while
the oscillations have an effect on the neutrino emission and the heating rates,
flavor transformation alone does not lead to a successful explosion of this
progenitor in spherical symmetry.

At the present time even the most sophisticated, multi-dimensional
simulations of core-collapse supernovae do not (self-consistently) include
neutrino flavor transformation. This physics is missing despite the importance
of neutrinos in the core-collapse explosion paradigm. Because of this
dependence, any flavor transformation that occurs in the region between the
proto-neutron star and the shock could result in major effects upon the
dynamics of the explosion. We present the first hydrodynamic core-collapse
supernova simulation which simultaneously includes flavor transformation of the
free-streaming neutrinos in the neutrino transport. These oscillation
calculations are dynamically updated and evolve self-consistently alongside the
hydrodynamics. Using a $M=20;{rm M_{odot}}$ progenitor, we find that while
the oscillations have an effect on the neutrino emission and the heating rates,
flavor transformation alone does not lead to a successful explosion of this
progenitor in spherical symmetry.

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