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Neutrino-nucleon scattering rate in proto-neutron star matter

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Neutrino-nucleon scattering rate in proto-neutron star matter

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dc.contributor.author Mornas, L.
dc.contributor.author Pérez Cañellas, Armando
dc.date.accessioned 2014-02-17T13:19:51Z
dc.date.available 2014-02-17T13:19:51Z
dc.date.issued 2002
dc.identifier.citation Mornas, L. Pérez Cañellas, Armando 2002 Neutrino-nucleon scattering rate in proto-neutron star matter European Physical Journal A 13 3 383 397
dc.identifier.uri http://hdl.handle.net/10550/32986
dc.description.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 supornova explosion and proto-neutron star cooling, we study the evolution of the neutrino mean free path as a function of density, proton-noutron 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(l) 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.
dc.relation.ispartof European Physical Journal A, 2002, vol. 13, num. 3, p. 383-397
dc.subject Partícules (Física nuclear)
dc.title Neutrino-nucleon scattering rate in proto-neutron star matter
dc.type journal article es_ES
dc.date.updated 2014-02-17T13:19:51Z
dc.identifier.doi 10.1007/s10050-002-8767-4
dc.identifier.idgrec 093317
dc.rights.accessRights open access es_ES
dc.identifier.url 10.1007/s10050-002-8767-4

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