Neutrino scattering rates in neutron star matter with Δ isobars

Physics

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Nuclear Matter Aspects Of Neutron Stars, Neutron Stars, Nuclear Matter, Neutrino Interactions

Scientific paper

We take the Δ-isobar degrees of freedom into account in neutron star matter and evaluate their contributions to neutrino scattering cross sections and mean free paths. The neutron star matter is described by means of an effective hadronic model in the relativistic mean-field approximation. It is found that Δ isobars may be present in neutron stars. The electron chemical potential does not decrease and the neutrino abundance does not increase with the increase of the density when neutrinos are trapped in the matter with Δ isobars. The large vector coupling constant between the Δ- and neutrino and the high spin of the Δ influence significantly the neutrino scattering cross section and lead the contribution of the Δ- to the dominance of the scattering rates. In neutrino-trapped case, the presence of Δs causes the neutrino mean free path to decrease drastically compared to that in the matter in which baryons are only nucleons.

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