New equations of state constrained by nuclear physics, observations, and QCD calculations of high-density nuclear matter. (arXiv:2009.08885v3 [nucl-th] UPDATED)

New equations of state constrained by nuclear physics, observations, and QCD calculations of high-density nuclear matter. (arXiv:2009.08885v3 [nucl-th] UPDATED)
<a href="http://arxiv.org/find/nucl-th/1/au:+Huth_S/0/1/0/all/0/1">S. Huth</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Wellenhofer_C/0/1/0/all/0/1">C. Wellenhofer</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Schwenk_A/0/1/0/all/0/1">A. Schwenk</a>

We present new equations of state for applications in core-collapse supernova
and neutron star merger simulations. We start by introducing an effective mass
parametrization that is fit to recent microscopic calculations up to twice
saturation density. This is important to capture the predicted thermal effects,
which have been shown to determine the proto-neutron star contraction in
supernova simulations. The parameter range of the energy-density functional
underlying the equation of state is constrained by chiral effective field
theory results at nuclear densities as well as by functional renormalization
group computations at high densities based on QCD. We further implement
observational constraints from measurements of heavy neutron stars, the
gravitational wave signal of GW170817, and from the recent NICER results.
Finally, we study the resulting allowed ranges for the equation of state and
for properties of neutron stars, including the predicted ranges for the neutron
star radius and maximum mass.

We present new equations of state for applications in core-collapse supernova
and neutron star merger simulations. We start by introducing an effective mass
parametrization that is fit to recent microscopic calculations up to twice
saturation density. This is important to capture the predicted thermal effects,
which have been shown to determine the proto-neutron star contraction in
supernova simulations. The parameter range of the energy-density functional
underlying the equation of state is constrained by chiral effective field
theory results at nuclear densities as well as by functional renormalization
group computations at high densities based on QCD. We further implement
observational constraints from measurements of heavy neutron stars, the
gravitational wave signal of GW170817, and from the recent NICER results.
Finally, we study the resulting allowed ranges for the equation of state and
for properties of neutron stars, including the predicted ranges for the neutron
star radius and maximum mass.

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