Mirror dark matter admixture via mutual mean-field shifts softens the nuclear EOS, raises central densities, lowers maximum masses, and moves the direct Urca onset to higher or lower masses depending on symmetry-energy stiffness.
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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.
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A self-consistent single-fluid framework for neutron stars admixed with mirror dark matter
Mirror dark matter admixture via mutual mean-field shifts softens the nuclear EOS, raises central densities, lowers maximum masses, and moves the direct Urca onset to higher or lower masses depending on symmetry-energy stiffness.
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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.