Improved neutrino-nucleon interactions in dense and hot matter for numerical simulations
Résumé
Neutrinos play an important role in compact star astrophysics:
neutrino-heating is one of the main ingredients in core-collapse
supernovae, neutrino-matter interactions determine the composition
of matter in binary neutron star mergers and have among others a
strong impact on conditions for heavy element nucleosynthesis and
neutron star cooling is dominated by neutrino emission except for
very old stars. Many works in the last decades have shown that in
dense matter medium effects considerably change the neutrino-matter
interaction rates, whereas many astrophysical simulations use
analytic approximations which are often far from reproducing more
complete calculations. In this work we present a scheme which allows
to incorporate improved rates, for charged current interactions,
into simulations and show as an example some results for
core-collapse supernovae, where a noticeable difference is found in
the location of the neutrinospheres of the low-energy neutrinos in
the early post-bounce phase.
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