Fluid modes of axisymmetric neutron stars

Oscillation modes of axisymmetric neutron stars (NSs) are computed in the framework of general relativity (GR) and by use of linearized perturbation theory. Applying the Cowling approximation, the mode calculation forms an eigenvalue problem which is then solved using polytropic equations of state. We compare the resulting pressure modes with the literature and find satisfying agreement. This work is the first step towards calculating the complete oscillation mode spectrum of rapidly rotating neutron stars