Relativistic Hartree-Fock calculations of charged-current neutrino opacities reveal large discrepancies and a substantial shift in medium-dependent modifications compared to standard relativistic mean-field models.
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Axial w-mode frequencies of anisotropic neutron stars decrease monotonically with mass, depend approximately linearly on compactness with anisotropy modifying slope and intercept, damping times increase with mass, and empirical expressions are given for both as functions of compactness and anisotrop
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Charged-current neutrino opacity within the relativistic Hartree-Fock framework for astrophysical simulations of core-collapse supernovae and binary neutron star mergers
Relativistic Hartree-Fock calculations of charged-current neutrino opacities reveal large discrepancies and a substantial shift in medium-dependent modifications compared to standard relativistic mean-field models.
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Axial $w$-modes of anisotropic neutron stars
Axial w-mode frequencies of anisotropic neutron stars decrease monotonically with mass, depend approximately linearly on compactness with anisotropy modifying slope and intercept, damping times increase with mass, and empirical expressions are given for both as functions of compactness and anisotrop