| Abstract
| - We examine radial oscillations of superfluid neutron stars at finite internal temperatures. For this purpose, we generalize the description of relativistic superfluid hydrodynamics to the case of superfluid mixtures. We show that in a neutron star, at hydrostatic and beta-equilibrium, the redshifted temperature gradient is smoothed out by neutron superfluidity (but not by proton superfluidity). We calculate radial oscillation modes of neutron stars assuming ‘frozen’ nuclear composition in the pulsating matter. The resulting pulsation frequencies show a strong temperature dependence in the temperature range (0.1−1) Tcn, where Tcn is the critical temperature of neutron superfluidity. Combining our results with thermal evolution, we obtain a significant evolution of the pulsation spectrum, associated with highly efficient Cooper pairing neutrino emission, for 20 yr after superfluidity onset.
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