Charged current neutrino interactions in core-collapse supernovae in a virial expansion

TL;DR

This paper calculates the energy shifts in neutrino interactions within supernovae using a virial expansion, revealing larger effects than mean field models and impacting neutrino energies and luminosities during supernovae.

Contribution

It introduces a model-independent virial expansion approach to compute energy shifts, showing these are significantly larger than previous mean field predictions.

Findings

nergy shift elta U is larger at low densities than mean field models.

elta U increases nti u_e energies in supernovae.

elta U decreases  u_e luminosity in simulations.

Abstract

Core-collapse supernovae may depend sensitively on charged current neutrino interactions in warm, low density neutron rich matter. A proton in neutron rich matter is more tightly bound than is a neutron. This energy shift \Delta U increases the electron energy in \nu_e + n --> p + e, increasing the available phase space and absorption cross section. Likewise \Delta U decreases the positron energy in \bar \nu_e + p --> n + e^+, decreasing the phase space and cross section. We have calculated \Delta U using a model independent virial expansion and we find \Delta U is much larger, at low densities, than the predictions of many mean field models. Therefore \Delta U could have a significant impact on charged current neutrino interactions in supernovae. Preliminary simulations of the accretion phase of core-collapse supernovae find that \Delta U increases \bar \nu_e energies and decreases the \nu_e luminosity.