Maximum mass of compact stars from gravitational wave events with finite-temperature equations of state. (arXiv:2102.00988v2 [astro-ph.HE] UPDATED)

Maximum mass of compact stars from gravitational wave events with finite-temperature equations of state. (arXiv:2102.00988v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Khadkikar_S/0/1/0/all/0/1">Sanika Khadkikar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raduta_A/0/1/0/all/0/1">Adriana R. Raduta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oertel_M/0/1/0/all/0/1">Micaela Oertel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sedrakian_A/0/1/0/all/0/1">Armen Sedrakian</a>

We conjecture and verify a set of universal relations between global
parameters of hot and fast-rotating compact stars, including a relation
connecting the masses of the mass-shedding (Kepler) and static configurations.
We apply these relations to the GW170817 event by adopting the scenario in
which a hypermassive compact star remnant formed in a merger evolves into a
supramassive compact star that collapses into a black hole once the stability
line for such stars is crossed. We deduce an upper limit on the maximum mass of
static, cold neutron stars $ 2.15^{+0.10}_{-0.07}le M^star_{mathrm{TOV}} le
2.24^{+0.12}_{-0.10} $ for the typical range of entropy per baryon $2 le S/A
le 3$ and electron fraction $Y_e = 0.1$ characterizing the hot hypermassive
star. Our result implies that accounting for the finite temperature of the
merger remnant relaxes previously derived constraints on the value of the
maximum mass of a cold, static compact star.

We conjecture and verify a set of universal relations between global
parameters of hot and fast-rotating compact stars, including a relation
connecting the masses of the mass-shedding (Kepler) and static configurations.
We apply these relations to the GW170817 event by adopting the scenario in
which a hypermassive compact star remnant formed in a merger evolves into a
supramassive compact star that collapses into a black hole once the stability
line for such stars is crossed. We deduce an upper limit on the maximum mass of
static, cold neutron stars $ 2.15^{+0.10}_{-0.07}le M^star_{mathrm{TOV}} le
2.24^{+0.12}_{-0.10} $ for the typical range of entropy per baryon $2 le S/A
le 3$ and electron fraction $Y_e = 0.1$ characterizing the hot hypermassive
star. Our result implies that accounting for the finite temperature of the
merger remnant relaxes previously derived constraints on the value of the
maximum mass of a cold, static compact star.

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