Mass and radius of the most massive neutron star: The probe of the equation of state and perturbative QCD
arxiv(2023)
摘要
Recently, an association of GW190425 and FRB 20190425A had been claimed and a
highly magnetized neutron star (NS) remnant was speculated. Given the ∼
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_ TOV) of the nonrotating NS is ≈
2.77M_⊙, which is strongly in tension with the relatively low M_
TOV≈ 2.25M_⊙ 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_ 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_ 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_ TOV and/or R_ 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_ 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_ TOV≈ 2.2M_⊙ 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.
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