A rescaling algorithm for artificial atmospheres achieves exact mass and electron number conservation to round-off precision in binary neutron star merger simulations.
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Any stand-alone dissipative hydrodynamic EFT is acausal; causal UV completions exist that preserve the exact IR hydrodynamic mode for subluminal sound speed and finite gradient-expansion radius.
High-resolution GR neutrino-radiation MHD simulation of 1.35-1.35 Msun BNS merger shows KHI-driven B-field amplification to magnetar levels (~10^50 erg, factor >=316) in 3 ms post-merger.
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.
Inelastic neutrino-electron scattering in hypermassive neutron star simulations increases disc mass by 75% and ejecta mass by 18% with higher neutrino luminosities, while electron-positron annihilation shows no significant impact.
citing papers explorer
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Exact Mass Conservation in Binary Neutron Star Merger Simulations
A rescaling algorithm for artificial atmospheres achieves exact mass and electron number conservation to round-off precision in binary neutron star merger simulations.
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Causal UV completions of relativistic hydrodynamics
Any stand-alone dissipative hydrodynamic EFT is acausal; causal UV completions exist that preserve the exact IR hydrodynamic mode for subluminal sound speed and finite gradient-expansion radius.
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A magnetar formation in binary neutron star merger
High-resolution GR neutrino-radiation MHD simulation of 1.35-1.35 Msun BNS merger shows KHI-driven B-field amplification to magnetar levels (~10^50 erg, factor >=316) in 3 ms post-merger.
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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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Influence of neutrino-electron scattering and neutrino-pair annihilation on hypermassive neutron star
Inelastic neutrino-electron scattering in hypermassive neutron star simulations increases disc mass by 75% and ejecta mass by 18% with higher neutrino luminosities, while electron-positron annihilation shows no significant impact.