Compiled properties of nucleonic matter and nuclear and neutron star models from nonrelativistic and relativistic interactions

Sun, Boyang; Bhattiprolu, Saketh; Lattimer, James M.

doi:10.1103/physrevc.109.055801

Cited by 6 publications

(1 citation statement)

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“…In fact, if one treats the results from the PREX and CREX experiments with equal weight, one finds that only nuclear interactions with symmetry energy parameters J = 32.2 ± 1.7 MeV and L = 52.7 ± 13.2 MeV (Lattimer 2023) can accommodate both experiments simultaneously (J and L being the symmetry energy and its slope at nuclear saturation density). In addition, the LHC measurement implies L ; 70 ± 40 MeV (Sun et al 2024). In comparison, nuclear mass fitting with a wide variety of both nonrelativistic and relativistic nuclear interactions yields J = 32.5 ± 2.1 MeV and L = 57.7 ± 20.7 MeV.…”

Section: Eos Implicationsmentioning

confidence: 95%

A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715

Choudhury,

Salmi,

Vinciguerra

et al. 2024

ApJL

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We report Bayesian inference of the mass, radius, and hot X-ray emitting region properties—using data from the Neutron Star Interior Composition ExploreR (NICER)—for the brightest rotation-powered millisecond X-ray pulsar, PSR J0437−4715. Our modeling is conditional on informative tight priors on mass, distance, and binary inclination obtained from radio pulsar timing using the Parkes Pulsar Timing Array (PPTA; Reardon et al.), and we use NICER background models to constrain the nonsource background, cross-checking with data from XMM-Newton. We assume two distinct hot emitting regions and various parameterized hot region geometries that are defined in terms of overlapping circles; while simplified, these capture many of the possibilities suggested by detailed modeling of return current heating. For the preferred model identified by our analysis, we infer a mass of M = 1.418 ± 0.037 M ⊙ (largely informed by the PPTA mass prior) and an equatorial radius of R = 11.36 − 0.63 + 0.95 km, each reported as the posterior credible interval bounded by the 16% and 84% quantiles. This radius favors softer dense matter equations of state and is highly consistent with constraints derived from gravitational wave measurements of neutron star binary mergers. The hot regions are inferred to be nonantipodal and hence inconsistent with a pure centered dipole magnetic field.

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Section: Eos Implicationsmentioning

confidence: 95%