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.
Title resolution pending
15 Pith papers cite this work. Polarity classification is still indexing.
15
Pith papers citing it
citation-role summary
background 2
citation-polarity summary
roles
background 2representative citing papers
Bayesian analysis of a smooth hadron-quark crossover EOS finds current observations tightly constrain the density dependence of nuclear symmetry energy while leaving highest-density hadronic and quark-matter parameters only weakly constrained.
A constrained Gaussian-process bridge prior generates model-agnostic, nonparametric, thermodynamically consistent priors for neutron-star equation-of-state inference.
Amortized neural posterior estimation reproduces nested sampling constraints on RMF couplings for neutron-star EOS with no bias and generates 30,000 samples in 2.5 seconds.
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.
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.
A centered swept-back multipolar magnetic field up to octupole order reproduces the bolometric thermal X-ray light curve of MSP J0030+0451.
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.
Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.
A controlled two-parameter deformation in linear f(Q) gravity with gravitational decoupling enlarges the stellar mass window for compact objects while satisfying causality and regularity.
Neutron star observations, especially the heaviest known pulsar masses and GW170817 tidal deformability, provide the strongest restrictions on the allowed cold dense matter equation of state.
A double-polytropic EOS family is identified that satisfies multimessenger constraints with M_max around 2.45 solar masses, R_1.4 of 11.3 km, and Lambda_1.4 between 485-512 while remaining causal.
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.
citing papers explorer
-
GPU-Accelerated X-ray Pulse Profile Modeling
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.
-
Constrained Gaussian-process bridge prior for neutron-star equation-of-state inference
A constrained Gaussian-process bridge prior generates model-agnostic, nonparametric, thermodynamically consistent priors for neutron-star equation-of-state inference.
-
Amortized Simulation-Based Inference of Relativistic Mean-Field Couplings for Neutron-Star Equations of State
Amortized neural posterior estimation reproduces nested sampling constraints on RMF couplings for neutron-star EOS with no bias and generates 30,000 samples in 2.5 seconds.
-
Pulse profile modelling of the 2024 outburst of the accreting millisecond pulsar SRGA J144459.2-604207
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.
-
The swept-back multipolar magnetic field of neutron stars: Application to NICER MSP J0030+0451
A centered swept-back multipolar magnetic field up to octupole order reproduces the bolometric thermal X-ray light curve of MSP J0030+0451.
-
Reconstruction of fast-rotating neutron star observables with the neural network
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.
-
Bayesian analysis of the shear modulus in the neutron-star crust
Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.
-
Astrophysical constraints on the cold equation of state of the strongly interacting matter
Neutron star observations, especially the heaviest known pulsar masses and GW170817 tidal deformability, provide the strongest restrictions on the allowed cold dense matter equation of state.
-
An Analytical Toy Equation of State for Neutron Stars Consistent with Current Observations
A double-polytropic EOS family is identified that satisfies multimessenger constraints with M_max around 2.45 solar masses, R_1.4 of 11.3 km, and Lambda_1.4 between 485-512 while remaining causal.