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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21 Pith papers cite this work, alongside 1,134 external citations. Polarity classification is still indexing.
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A constrained Gaussian-process bridge prior generates model-agnostic, nonparametric, thermodynamically consistent priors for neutron-star equation-of-state inference.
Neural-network surrogate accelerated MCMC infers multipolar magnetic field parameters for PSR J0740+6620 from NICER data, finding broad multimodal posteriors and disfavoring a zero-offset model.
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.
A semi-supervised VAE trained on Skyrme EOS data reconstructs equations of state with mean absolute percentage errors under 0.14% using two supervised observables (M_max, R_1.4) and one variational latent variable.
Joint MCMC analysis of Chandra and XMM-Newton quiescent 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 when distance uncertainty is included.
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.
Mass-gap compact objects could be hybrid stars only with very early deconfinement and stiff quark matter; confirming 1.4 M⊙ twin stars would cap hybrid-star maximum mass below 2.2 M⊙.
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.
Multi-messenger observations of neutron stars imply L=42.6–52 MeV (piecewise polytrope) or 44.2–56.7 MeV (speed-of-sound) at 68% credibility, and show pQCD constraints barely change the posterior EOS.
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
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.
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.
-
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.
-
Multipolar Magnetic-Field Inference for PSR J0740+6620 with Neural-Network-Accelerated NICER Pulse-Profile Modeling
Neural-network surrogate accelerated MCMC infers multipolar magnetic field parameters for PSR J0740+6620 from NICER data, finding broad multimodal posteriors and disfavoring a zero-offset model.
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As above, so below: assessing extremeness of the neutron-star equation of state based on the unstable branch
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.
-
A Semi-Supervised Variational Autoencoder for Generating Neutron Star Equations of State
A semi-supervised VAE trained on Skyrme EOS data reconstructs equations of state with mean absolute percentage errors under 0.14% using two supervised observables (M_max, R_1.4) and one variational latent variable.
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Neutron Star Mass-Radius Constraints for EXO 0748$-$676 from 2008-2025 Quiescent X-ray Spectra
Joint MCMC analysis of Chandra and XMM-Newton quiescent 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 when distance uncertainty is included.
-
Holographic Thermodynamic Signatures of Simpson--Visser--AdS Black Holes
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.
-
Hybrid stars among mass gap objects are excluded by twin stars at $1.4\,M_\odot$
Mass-gap compact objects could be hybrid stars only with very early deconfinement and stiff quark matter; confirming 1.4 M⊙ twin stars would cap hybrid-star maximum mass below 2.2 M⊙.
-
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.
-
Astrophysics equation of state inference with Bayesian chiral effective field theory uncertainties
Multi-messenger observations of neutron stars imply L=42.6–52 MeV (piecewise polytrope) or 44.2–56.7 MeV (speed-of-sound) at 68% credibility, and show pQCD constraints barely change the posterior EOS.
-
Nonlinear electrodynamics in magnetars: systematic effects on radius constraints and timing analysis
NLED alters photon propagation near magnetars, producing ~10% errors in inferred radii via ray-tracing and a minimal ~350 ns travel-time delay.
-
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.
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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.
-
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 inferences on covariant density functionals from multimessenger astrophysical data: Influences of parametrizations of density dependent couplings
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
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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.
-
Impact of the equation of state on core collapse supernovae I: the low-$T/|W|$ instability
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.
-
Estimation of neutron star mass and radius of FRB 20240114A by identification of crustal oscillations
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.
-
Nuclear Physics of Binary Neutron Star Mergers
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 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.
- On the Possibility of a Strong First-Order Phase Transition in Neutron Stars