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Published in

Oxford University Press, Monthly Notices of the Royal Astronomical Society, 1(505), p. 939-946, 2021

DOI: 10.1093/mnras/stab1348

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

Journal article published in 2021 by E. Préau, A. Pascal, J. Novak ORCID, M. Oertel ORCID
This paper was not found in any repository, but could be made available legally by the author.
This paper was not found in any repository, but could be made available legally by the author.

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Data provided by SHERPA/RoMEO

Abstract

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 parametrized 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. Our results suggest 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.