2018 Impact factor 2.481
Hadrons and Nuclei


Eur. Phys. J. A 13, 383-397 (2002)

Neutrino-nucleon scattering rate in proto-neutron star matter

L. Mornas1 and A. Pérez2

1  Departamento de Física, Universidad de Oviedo, Av.da Calvo Sotelo, E-33007 Oviedo (Asturias) Spain
2  Departamento de Física Teórica, Universidad de Valencia, E-46100 Burjassot (Valencia), Spain

lysiane@pinon.ccu.uniovi.es

(Received: 27 June 2001 / Revised version: 14 January 2002 Communicated by V. Vento)

Abstract
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 $\sigma$, $\omega$, $\pi$, $\rho$ and $\delta$ 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.

© Società Italiana di Fisica, Springer-Verlag 2002