Heat diffusion introduces a distinct thermal mode sector in viscous star oscillations that transitions to propagating behavior above a critical overtone, realizing finite-size relativistic second sound.
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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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Radial Oscillations of Viscous Stars at Finite Temperature
Heat diffusion introduces a distinct thermal mode sector in viscous star oscillations that transitions to propagating behavior above a critical overtone, realizing finite-size relativistic second sound.
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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.