Eur. Phys. J. A 13, 383-397 (2002)
Neutrino-nucleon scattering rate in proto-neutron star matter
L. Mornas1 and A. Pérez21 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
,
,
,
and
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.
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
