Improved neutrino-nucleon interactions in dense and hot matter for numerical simulations. (arXiv:2003.02152v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Oertel_M/0/1/0/all/0/1">Micaela Oertel</a> (LUTH (UMR_8102)), <a href="http://arxiv.org/find/astro-ph/1/au:+Pascal_A/0/1/0/all/0/1">Aurélien Pascal</a> (LUTH (UMR_8102)), <a href="http://arxiv.org/find/astro-ph/1/au:+Mancini_M/0/1/0/all/0/1">Marco Mancini</a> (LUTH (UMR_8102)), <a href="http://arxiv.org/find/astro-ph/1/au:+Novak_J/0/1/0/all/0/1">Jerome Novak</a> (LUTH (UMR_8102))
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.
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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