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.
Huanget al., (2024), arXiv:2411.14615 [astro-ph.HE]
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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.
Authors define U-spin symmetry energy for hyperonic matter, constrain it via Bayesian inference from nuclear and astrophysical data, and conclude Lambda hyperons likely emerge between 2-5 n0 but vanish above 5 n0 with over 50% posterior probability.
Bayesian inference on observational data yields shear viscosity timescale τ_s=(4.99^{+0.49}_{-0.52})×10^8 T^{5/3} s and bulk viscosity timescale for two-layer hybrid stars, giving frequency minima of 451.87 Hz and 517.47 Hz that explain stability of pulsars including XTE J0929-314.
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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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U-spin symmetry energy and hyperon puzzle
Authors define U-spin symmetry energy for hyperonic matter, constrain it via Bayesian inference from nuclear and astrophysical data, and conclude Lambda hyperons likely emerge between 2-5 n0 but vanish above 5 n0 with over 50% posterior probability.