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In this paper we compute general-relativistic polytropic models simulatingrigidly rotating, pulsating neutron stars. These relativistic compact objects,with a radius of $\sim 10 \, \mathrm{km}$ and mass between $\sim 1.4$ and $3.2$solar masses, are closely related to pulsars. We emphasize on computing thechange in the pulsation eigenfrequencies owing to a rigid rotation, which, inturn, is a decisive issue for studying stability of such objects. In ourcomputations, we keep rotational perturbation terms of up to second order inthe angular velocity.

Quasi-radial modes of pulsating neutron stars: numerical results for general-relativistic rigidly rotating polytropic models