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.
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6 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
representative citing papers
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 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 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.
citing papers explorer
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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.
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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.
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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.
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Combining the Mass--Radius Posteriors of J0030+0451 Allowing for Unknown Model Systematics
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.