Neutrino-nucleon scattering rates in protoneutron stars and nuclear correlations in the spin S = 1 channel

Abstract

The neutrino-nucleon cross-section is calculated in dense nuclear matter at finite temperature, in view of applications to supernovae and protoneutron stars. The main contribution to this parameter is provided by the axial response function. Nuclear correlations play an important role: while the v-N crosssection is usually reduced by correlations, a collective mode in the spin S = 1 channel may be excited. In that case, the cross-section diverges and the neutrino mean free path would be drastically reduced. The predictions of various models of the nuclear force commonly used in the literature are compared in relation with a possible spin instability. While Skyrme or Gogny forces lead to attraction in this channel, variational or Brueckner-Hartree-Fock calculations predict a repulsive contribution. An interesting alternative appears to be the density-dependent M3Y interaction.