Abstract
In this article the role of the supersaturation density equation of state (EOS) is explored in simulations of failed core-collapse supernova explosions. Therefore the nuclear EOS is extended via a one-parameter excluded volume description for baryons, taking into account their finite and increasing volume with increasing density in excess of saturation density. Parameters are selected such that the resulting supernova EOS represent extreme cases, with high pressure variations at supersaturation density which feature extreme stiff and soft EOS variants of the reference case, i.e. without excluded volume corrections. Unlike in the interior of neutron stars with central densities in excess of several times saturation density, central densities of core-collapse supernovae reach only slightly above saturation density. Hence, the impact of the supersaturation density EOS on the supernova dynamics as well as the neutrino signal is found to be negligible. It is mainly determined from the low- and intermediate-density domain, which is left unmodified within this generalized excluded volume approach.
Highlights
A neutron star is born in the violent event of a corecollapse supernova explosion of a star more massive than about 9 M
I follow a different approach by modifying only the supersaturation density equation of state (EOS) of a well selected nuclear relativistic mean-field (RMF) model [28,29] that has been widely explored in the core-collapse supernova community (c.f. ref. [30])
A (2016) 52: 54 proach introduced in ref. [31] is employed here for densities in excess of nuclear saturation density (ρ0). It modifies the available volume of the nucleon gas which effectively adjusts the baryon EOS. This setup will allow for a direct identification of the high-density EOS impact on the supernova dynamics as well as the neutrino signal
Summary
A neutron star is born in the violent event of a corecollapse supernova explosion of a star more massive than about 9 M. I follow a different approach by modifying only the supersaturation density EOS of a well selected nuclear relativistic mean-field (RMF) model [28,29] that has been widely explored in the core-collapse supernova community It modifies the available volume of the nucleon gas which effectively adjusts the baryon EOS This setup will allow for a direct identification of the high-density EOS impact on the supernova dynamics as well as the neutrino signal. 3 briefly introduces the excluded-volume mechanism of [31] that is applied to modify the supersaturation density EOS These are included in simulations of failed core-collapse supernova simulations which are analyzed in sect.
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