First public GPU-accelerated pulse-profile modeling code for X-ray millisecond pulsars that delivers 10^3–10^4 speedups to 2–5 ms per evaluation at 10^{-3} relative accuracy and removes an interpolation bias in atmosphere tables.
( year 2021 ), month Sep
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A constrained Gaussian-process bridge prior generates model-agnostic, nonparametric, thermodynamically consistent priors for neutron-star equation-of-state inference.
Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable stars.
Bayesian analysis favors a strong first-order phase transition in cold dense QCD matter whose onset lies above the central density of the most massive observed neutron stars.
Simpson-Visser regularization of Schwarzschild-AdS black holes yields a van der Waals-type temperature branch structure with three coexisting equilibria and topological charge W=+1 for regularization parameter below 1/sqrt(24), distinguishing it from the Schwarzschild-AdS case.
Joint NICER+IXPE pulse-profile modeling of SRGA J144459.2-604207 favors large neutron-star mass and radius with two independent hotspots but shows strong sensitivity to joint-analysis methodology.
Bayesian EOS inference with χEFT uncertainty priors and LIGO/NICER data yields posteriors consistent with prior work, a stiffening above 3n0, negligible pQCD impact, and an inferred symmetry-energy slope L of 42.6-56.7 MeV.
NLED alters photon propagation near magnetars, producing ~10% errors in inferred radii via ray-tracing and a minimal ~350 ns travel-time delay.
A centered swept-back multipolar magnetic field up to octupole order reproduces the bolometric thermal X-ray light curve of MSP J0030+0451.
A Bayesian combination of eight M-R posteriors for PSR J0030+0451 yields M = 1.46^{+0.09}_{-0.08} M_⊙, R = 12.69^{+0.64}_{-0.55} km while marginalizing over unknown model systematics.
Causal convolutional neural networks reconstruct neutron star observables for static, Keplerian, and rotating configurations in about 50 milliseconds per equation of state, compared to 30 minutes with traditional RNS calculations.
Different parametrizations of density dependence in covariant density functionals produce significant variations in the high-density equation of state and symmetry energy, with rational-function forms providing flexibility when saturation properties are adjusted and constrained by multimessenger ast
Global MCMC fit to Chandra and XMM-Newton spectra yields M = 1.77^{+0.17}_{-0.22} M_⊙ and R = 12.62^{+0.56}_{-0.74} km at 7.1 kpc, with conservative ranges 1.41-2.11 M_⊙ and 10.15-15.13 km favoring stiff EOS.
Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.
Simulations show the low-T/|W| instability develops robustly across five nuclear EOS in a rapidly rotating 35 M⊙ progenitor, with dominant GW frequency correlating to PNS compactness and stiffness.
Matching FRB QPOs to crustal modes constrains the neutron star mass to 1.00-1.76 solar masses, radius to ~13 km, and nuclear symmetry energy slope L to 59.5-96.8 MeV.
Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.
Relativistic mean-field models provide a unified framework for describing bulk nuclear properties and the equation of state of dense neutron-rich matter in neutron stars.
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Relativistic mean-field models of neutron-rich matter
Relativistic mean-field models provide a unified framework for describing bulk nuclear properties and the equation of state of dense neutron-rich matter in neutron stars.