Mass and radius of the most massive neutron star: The probe of the equation of state and perturbative QCD

Abstract

Recently, an association of GW190425 and FRB 20190425A had been claimed and a highly magnetized neutron star (NS) remnant was speculated. Given the $\sim 2.5$-h delay of the occurrence of FRB 20190425A, a uniformly rotating supramassive magnetar is favored since the differential rotation would have been promptly terminated by the magnetic braking. The required maximum gravitational mass ($M_{\mathrm{TOV}}$) of the nonrotating NS is $\approx 2.77M_{\odot }$, which is strongly in tension with the relatively low $M_{\mathrm{TOV}}\approx 2.25M_{\odot }$ obtained in current equation of state (EOS) constraints incorporating perturbative quantum chromodynamics (pQCD) information. However, the current mass-radius and mass-tidal deformability measurements of NSs alone do not convincingly exclude the high $M_{\mathrm{TOV}}$ possibility. By performing EOS constraints with mock measurements, we find that with a $2\%$ determination for the radius of PSR J0740+6620-like NS it is possible to distinguish between the low and high $M_{\mathrm{TOV}}$ scenarios. We further explore the prospect to resolve the issue of the appropriate density to impose the pQCD constraints with future massive NS observations or determinations of $M_{\mathrm{TOV}}$ and/or $R_{\mathrm{TOV}}$. It turns out that measuring the radius of a PSR J0740+6620-like NS is insufficient to probe the EOSs around 5 nuclear saturation density, where the information from pQCD becomes relevant. The additional precise $M_{\mathrm{TOV}}$ measurements anyhow could provide insights into the EOS at such a density. Indeed, supposing the central engine of GRB 170817A is a black hole formed via the collapse of a supramassive NS, the resulting $M_{\mathrm{TOV}}\approx 2.2M_{\odot }$ considerably softens the EOS at the center of the most massive NS, which is in favor of imposing the pQCD constraint at density beyond the one achievable in the NSs.

12 pages, 5 figures, PRD published

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• Phase transition and nuclear symmetry energy from neutron star observations: Constraints in light of PSR J0614--3329
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• The maximum mass and rotational kinetic energy of rapidly rotating neutron stars
• Updated estimates of post-merger gravitational wave energy released in GW170817 and the maximum neutron star mass