Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable stars.
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Hadronic pp collisions dominate pair loading via pion cascades in magnetar-like outflows from neutron star mergers, channeling magnetic energy into e± and seeding neutrinos up to ~300 MeV.
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.
citing papers explorer
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As above, so below: assessing extremeness of the neutron-star equation of state based on the unstable branch
Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable stars.
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Hadronic Processes, Plasma Evolution and Neutrino Emission in Magnetic Towers of Neutron-Star Merger Remnants
Hadronic pp collisions dominate pair loading via pion cascades in magnetar-like outflows from neutron star mergers, channeling magnetic energy into e± and seeding neutrinos up to ~300 MeV.
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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.