Are hypermassive neutron stars stable against a prompt collapse?

Differential rotation in neutron stars allows for significantly larger masses than rigid rotation. Some of those hypermassive objects are, however, unstable and collapse to a black hole immediately after formation. Yet, the exact threshold of dynamical stability is still unknown. In our work we expl...

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Bibliographic Details
Published inProceedings of the International Astronomical Union Vol. 16; no. S363; pp. 350 - 351
Main Authors Szewczyk, Paweł, Gondek-Rosińska, Dorota, Kolasa, Kamil, Mehta, Parita
Format Journal Article
LanguageEnglish
Published Cambridge, UK Cambridge University Press 01.06.2020
Subjects
Astronomy
Black holes
Differential rotation
Dynamic stability
Equations of state
Equilibrium
Gravitational waves
Neutron stars
Neutrons
Poster Paper
Stellar rotation
stability
supernova remnants
neutron stars
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Summary:Differential rotation in neutron stars allows for significantly larger masses than rigid rotation. Some of those hypermassive objects are, however, unstable and collapse to a black hole immediately after formation. Yet, the exact threshold of dynamical stability is still unknown. In our work we explore the limits on masses of neutron stars with various degrees of differential rotation which could be stable against a prompt collapse to a black hole by using turning-point (j-constant) criterion. We considered both spheroidal and quasi-toroidal differentially rotating neutron stars described by the polytropic equation of state. We find that massive configurations could be temporarily stabilized by differential rotation. Such objects are important sources of gravitational waves. Our results are a starting point for more detailed studies of stability using hydrodynamical codes.
ISSN:1743-9213
1743-9221
DOI:10.1017/S1743921322000977