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

被引：6

作者：

Preau, E. ^{[1
,2
]}

Pascal, A. ^{[1
]}

Novak, J. ^{[1
]}

Oertel, M. ^{[1
]}

机构：

[1] Univ Paris, Univ PSL, Observ Paris, Lab Univers & Theories, F-92190 Meudon, France

[2] Univ Paris, CNRS, Astroparticule & Cosmol, F-75013 Paris, France

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2021年 / 505卷 / 01期

关键词：

equation of state; methods: numerical; stars: neutron; GRAVITATIONAL-WAVE OBSERVATIONS; CORE-COLLAPSE SUPERNOVAE; EQUATION; ASTEROSEISMOLOGY; STATE; TESTS;

D O I：

10.1093/mnras/stab1348

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页码：939 / 946

页数：8

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