Seismology of superfluid neutron stars

An increasing amount of observational data provides us with more and more manifestations of neutron star (NS) oscillations. To interpret existing and future observations one needs to develop adequate models of oscillating NSs. Such models have to account for baryon pairing in stellar interiors. In my talk I will first discuss some general characteristics of oscillation modes in superfluid NSs, their spectra and dissipation timescales. I will then present some more details about two specific classes of oscillations called g-modes, which might excite resonantly during the neutron star inspirals, and about r-modes, which can serve as a powerful tool to probe the properties of superdense matter. Finally, I will consider possible imprints of superfluid oscillation modes in gravitational wave signal from neutron star inspirals.