First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.
Koehn et al., An overview of existing and new nuclear and astrophysical constraints on the equation of state of neutron-rich dense matter, (2024), arXiv:2402.04172 [astro-ph.HE]
4 Pith papers cite this work, alongside 9 external citations. Polarity classification is still indexing.
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Neutron dark decays modify the equation of state and either mildly suppress or strongly enhance bulk viscosity in neutron star merger conditions, depending on the in-medium decay rate.
PHQMD simulations with momentum-dependent potentials show that a soft momentum-dependent EoS calibrated to pA data reproduces experimental proton and cluster flows at midrapidity better than static EoS variants, while cluster formation method affects flow patterns.
Theoretical inputs and the 2 solar mass lower limit dominate neutron star equation of state constraints across most densities, while radius data refines low densities and higher masses affect wider ranges.
citing papers explorer
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Detection of relativistic orbital deformation from improved timing of PSR J1757$-$1854
First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.
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Bulk viscosity from neutron decays to dark baryons in neutron star matter
Neutron dark decays modify the equation of state and either mildly suppress or strongly enhance bulk viscosity in neutron star merger conditions, depending on the in-medium decay rate.
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Systematic study of flow of protons and light clusters in intermediate-energy heavy-ion collisions with momentum-dependent potentials
PHQMD simulations with momentum-dependent potentials show that a soft momentum-dependent EoS calibrated to pA data reproduces experimental proton and cluster flows at midrapidity better than static EoS variants, while cluster formation method affects flow patterns.
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Sensitivity of the Neutron Star Equation of State Inferences to Mass and Radius Measurements
Theoretical inputs and the 2 solar mass lower limit dominate neutron star equation of state constraints across most densities, while radius data refines low densities and higher masses affect wider ranges.