LightGBM and other regressors achieve R^{2}≈0.6–0.7 under random CV on CCSN GW catalogues but collapse to worse-than-mean performance under Leave-One-EoS-Out validation, exposing a generalisation gap for unseen EoS families.
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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.
Mirror dark matter fraction f_D in the range 0.12-0.88 reproduces the GW170817 tidal constraint and can reduce visible radii even when the ordinary-matter EOS yields no macroscopic quark core.
Strong proton superconductivity at high densities shuts down nucleon and hyperon direct Urca cooling, making kaon-induced Urca processes dominant and explaining cold massive neutron stars.
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The Generalization Gap in Machine Learning EoS Inference from Core-Collapse Supernova Gravitational Waves
LightGBM and other regressors achieve R^{2}≈0.6–0.7 under random CV on CCSN GW catalogues but collapse to worse-than-mean performance under Leave-One-EoS-Out validation, exposing a generalisation gap for unseen EoS families.
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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.
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Effects of Mirror Dark Matter on Neutron-Star Structure and Tidal Deformability
Mirror dark matter fraction f_D in the range 0.12-0.88 reproduces the GW170817 tidal constraint and can reduce visible radii even when the ordinary-matter EOS yields no macroscopic quark core.
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Cooling of Isolated Neutron Stars with Hyperon-mixed Kaon-Condensation Matter
Strong proton superconductivity at high densities shuts down nucleon and hyperon direct Urca cooling, making kaon-induced Urca processes dominant and explaining cold massive neutron stars.