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.
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A Kokkos-based C++ port of the SACRA numerical relativity code achieves ~10x speedup on GPU/APU over the Fortran CPU version while preserving waveform accuracy, pi-symmetry, and second-order convergence.
No sub-solar-mass compact-binary mergers were found in LIGO O4a data, giving 90% merger-rate upper limits of 110-10000 Gpc^-3 yr^-1 and weak new dark-matter constraints.
Molecular dynamics simulations produce a new equation of state P(n_B, T) for warm neutron star outer crusts with tabulated data and neural network parametrization on Zenodo.
Hybrid star models with constant sound speed quark matter match NICER data for PSR J0740+6620 and PSR J0030+0451 only when the energy density discontinuity at the phase transition is small and the quark sound speed is relatively high.
citing papers explorer
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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.
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SACRA-K: A Performance-Portable Numerical Relativity Code with Kokkos
A Kokkos-based C++ port of the SACRA numerical relativity code achieves ~10x speedup on GPU/APU over the Fortran CPU version while preserving waveform accuracy, pi-symmetry, and second-order convergence.
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Searches for Binary Mergers with Sub-solar Mass Components in Data from the First Part of LIGO--Virgo--KAGRA's Fourth Observing Run
No sub-solar-mass compact-binary mergers were found in LIGO O4a data, giving 90% merger-rate upper limits of 110-10000 Gpc^-3 yr^-1 and weak new dark-matter constraints.
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Equation of State for warm Neutron Star outer crusts
Molecular dynamics simulations produce a new equation of state P(n_B, T) for warm neutron star outer crusts with tabulated data and neural network parametrization on Zenodo.
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Can a hybrid star with constant sound speed parametrization explain the new NICER mass-radius measurements ?
Hybrid star models with constant sound speed quark matter match NICER data for PSR J0740+6620 and PSR J0030+0451 only when the energy density discontinuity at the phase transition is small and the quark sound speed is relatively high.