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.
Colloquium : Measuring the neutron star equation of state using x-ray timing
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
representative citing papers
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.
The (axial-)vector meson extended linear sigma model yields an equation of state for quark matter that satisfies astrophysical constraints on compact star masses and radii.
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.
-
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.
-
Compact star properties from an extended linear sigma model
The (axial-)vector meson extended linear sigma model yields an equation of state for quark matter that satisfies astrophysical constraints on compact star masses and radii.