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
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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.
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.
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.
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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.