What can be learned from a proto-neutron star's mass and radius?

Abstract

We make extensive numerical studies of masses and radii of proto-neutron stars during the first second after their birth in core-collapse supernova events. We use a quasi-static approach for the computation of proto-neutron star structure, built on parameterized entropy and electron fraction profiles, that are then evolved with neutrino cooling processes. We vary the equation of state of nuclear matter, the proto-neutron star mass and the parameters of the initial profiles, to take into account our ignorance of the supernova progenitor properties. We show that if masses and radii of a proto-neutron star can be determined in the first second after the birth, e.g. from gravitational wave emission, no information could be obtained on the corresponding cold neutron star and therefore on the cold nuclear equation of state. Similarly, it seems unlikely that any property of the proto-neutron star equation of state (hot and not beta-equilibrated) could be determined either, mostly due to the lack of information on the entropy, or equivalently temperature, distribution in such objects.

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Cited by in corpus (6)

• Universal relation for supernova gravitational waves
• EoS for hot neutron stars
• Unified neutron star EOSs and neutron star structures in RMF models
• Unified nuclear matter EOSs constrained by the in-medium balance in density-dependent covariant density functionals
• Spontaneous Scalarization in Proto-neutron Stars
• Properties and microscopic structures of dense stellar matter in RMF models