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Constraint on the maximum mass of neutron stars using GW170817 event

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arxiv 1905.03656 v3 pith:5Y3XAEOS submitted 2019-05-09 astro-ph.HE gr-qcnucl-th

Masaru Shibata , Enping Zhou , Kenta Kiuchi , Sho Fujibayashi This is my paper · ORCID
classification astro-ph.HEgr-qcnucl-th
keywords neutronstarsmassmaximumconstraintanalysisangularcold
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abstract

We revisit the constraint on the maximum mass of cold spherical neutron stars coming from the observational results of GW170817. We develop a new framework for the analysis by employing both energy and angular momentum conservation laws as well as solid results of latest numerical-relativity simulations and of neutron stars in equilibrium. The new analysis shows that the maximum mass of cold spherical neutron stars can be only weakly constrained as $M_{\rm max} \alt 2.3M_\odot$. Our present result illustrates that the merger remnant neutron star at the onset of collapse to a black hole is not necessarily rapidly rotating and shows that we have to take into account the angular momentum conservation law to impose the constraint on the maximum mass of neutron stars.

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Cited by 4 Pith papers

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  3. The error budget of binary neutron star merger simulations for configurations with high spin

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  4. Connecting GRBs from Binary Neutron Star Mergers to Nuclear Properties of Neutron Stars

    astro-ph.HE 2024-12 conditional novelty 6.0 of 10

    By matching population-synthesis predictions to the observed ratio of long to short GRBs from binary neutron star mergers, the authors infer that the long-short remnant transition lies near M_ls ~ 1.3 M_TOV.

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