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 ~10 km and
mass between ~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.
Share and Cite:
Geroyannis, V. and Tzelati, E. (2014) Quasi-Radial Modes of Pulsating Neutron Stars: Numerical Results for General-Relativistic Rigidly Rotating Polytropic Models.
International Journal of Astronomy and Astrophysics,
4, 453-463. doi:
10.4236/ijaa.2014.43041.
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