Gravitational wave asteroseismology with fast rotating neutron stars

During the birth of a proto-neutron star or the merging of two older compact stars, violent non-radial oscillations may be excited, resulting in the emission of significant amounts of gravitational radiation [1]. The detection of gravitational waves from oscillating neutron stars will allow the study of their interior, in the same way as helioseismology provides information about the interior of the Sun. It is expected that the identification of specific pulsation frequencies in the observational data will reveal the true properties of matter at densities that cannot be probed today by any other experiment. In this paper, we present new empirical relationships for mode-frequencies and damping times of the quadrupolar f -mode for rapidly rotating neutron stars, extending previous studies which deal with the non-rotating case [2‐4].