Abstract
Pulse profile modeling of X-ray data from the Neutron Star Interior Composition Explorer is now enabling precision inference of neutron star mass and radius. Combined with nuclear physics constraints from chiral effective field theory (χEFT), and masses and tidal deformabilities inferred from gravitational-wave detections of binary neutron star mergers, this has led to a steady improvement in our understanding of the dense matter equation of state (EOS). Here, we consider the impact of several new results: the radius measurement for the 1.42 M
⊙ pulsar PSR J0437−4715 presented by Choudhury et al., updates to the masses and radii of PSR J0740+6620 and PSR J0030+0451, and new χEFT results for neutron star matter up to 1.5 times nuclear saturation density. Using two different high-density EOS extensions—a piecewise-polytropic (PP) model and a model based on the speed of sound in a neutron star (CS)—we find the radius of a 1.4 M
⊙ (2.0 M
⊙) neutron star to be constrained to the 95% credible ranges
12.28
−
0.76
+
0.50
km (
12.33
−
1.34
+
0.70
km) for the PP model and
12.01
−
0.75
+
0.56
km (
11.55
−
1.09
+
0.94
km) for the CS model. The maximum neutron star mass is predicted to be
2.15
−
0.16
+
0.14
M
⊙ and
2.08
−
0.16
+
0.28
M
⊙ for the PP and CS models, respectively. We explore the sensitivity of our results to different orders and different densities up to which χEFT is used, and show how the astrophysical observations provide constraints for the pressure at intermediate densities. Moreover, we investigate the difference R
2.0 − R
1.4 of the radius of 2 M
⊙ and 1.4 M
⊙ neutron stars within our EOS inference.
