Neutrino-nucleon scattering rate in proto-neutron star matter

  • L. Mornas
  • A. Pérez


We present a calculation of the neutrino-nucleon scattering cross-section which takes into account the nuclear correlations in the relativistic random phase approximation (RPA). Our approach is based on a quantum-hadrodynamics model with exchange of σ, ω, π, ρ and δ mesons. In view of applications to neutrino transport in the final stages of supernova explosion and proto-neutron star cooling, we study the evolution of the neutrino mean free path as a function of density, proton-neutron asymmetry and temperature. Special attention was paid to the issues of renormalization of the Dirac sea, residual interactions in the tensor channel, coupling to the delta-meson and meson mixing. In contrast with the results of other authors, we find that the neutral-current process is not sensitive to the strength g' of the residual contact interaction. As a consequence, it is found that RPA corrections with respect to the mean-field approximation amount to only 10% to 15% at high density.

PACS. 26.60.+c Nuclear matter aspects of neutron stars – 13.15.+g Neutrino interactions – 24.10.Jv Relativistic models 


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Copyright information

© Società Italiana di Fisica and Springer-Verlag 2002

Authors and Affiliations

  • L. Mornas
    • 1
  • A. Pérez
    • 2
  1. 1.Departamento de Física, Universidad de Oviedo, Av.da Calvo Sotelo, E-33007 Oviedo (Asturias) SpainES
  2. 2.Departamento de Fısica Teórica, Universidad de Valencia, E-46100 Burjassot (Valencia), SpainES

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