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

Abstract

In this paper we compute general-relativistic polytropic models simulating rigidly 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 the change in the pulsation eigenfrequencies owing to a rigid rotation, which, in turn, is a decisive issue for studying stability of such objects. In our computations, we keep rotational perturbation terms of up to second order in the angular velocity.

v1 has been submitted to the International Journal of Astronomy and Astrophysics and accepted after revision; v2, i.e. the present version, is the revised E-print; 16 pages