Nuclear-Physics Multi-Messenger Astrophysics Constraints on the Neutron-Star Equation of State: Adding NICER's PSR J0740+6620 Measurement

TL;DR

This paper combines recent multi-messenger astrophysical data, including NICER's measurements of PSR J0740+6620, to refine constraints on the neutron-star equation of state and maximum mass, disfavoring strong phase transitions.

Contribution

It updates neutron-star equation of state constraints using new observational data, especially from PSR J0740+6620, integrating multiple astrophysical measurements for improved modeling.

Findings

Estimated neutron star radius: 11.94^{+0.76}_{-0.87} km for 1.4 solar masses

Disfavors strong first-order phase transitions inside neutron stars

Provides updated upper bounds on neutron star maximum mass

Abstract

In the past few years, new observations of neutron stars and neutron-star mergers have provided a wealth of data that allow one to constrain the equation of state of nuclear matter at densities above nuclear saturation density. However, most observations were based on neutron stars with masses of about 1.4 solar masses, probing densities up to $\sim$ 3-4 times the nuclear saturation density. Even higher densities are probed inside massive neutron stars such as PSR J0740+6620. Very recently, new radio observations provided an update to the mass estimate for PSR J0740+6620 and X-ray observations by the NICER and XMM telescopes constrained its radius. Based on these new measurements, we revisit our previous nuclear-physics multi-messenger astrophysics constraints and derive updated constraints on the equation of state describing the neutron-star interior. By combining astrophysical observations of two radio pulsars, two NICER measurements, the two gravitational-wave detections GW170817 and GW190425, detailed modeling of the kilonova AT2017gfo, as well as the gamma-ray burst GRB170817A, we are able to estimate the radius of a typical 1.4-solar mass neutron star to be $11.94^{+0.76}_{-0.87} \rm{km}$ at $90\%$ confidence. Our analysis allows us to revisit the upper bound on the maximum mass of neutron stars and disfavors the presence of a strong first-order phase transition from nuclear matter to exotic forms of matter, such as quark matter, inside neutron stars.