Non-axisymmetric oscillations of rapidly rotating relativistic stars by conformal flatness approximation

Abstract

We present a new numerical code to compute non-axisymmetric eigenmodes of rapidly rotating relativistic stars by adopting spatially conformally flat approximation of general relativity. The approximation suppresses the radiative degree of freedom of relativistic gravity and the field equations are cast into a set of elliptic equations. The code is tested against the low-order f- and p-modes of slowly rotating stars for which a good agreement is observed in frequencies computed by our new code and those computed by the full theory. Entire sequences of the low order counter-rotating f-modes are computed, which are susceptible to an instability driven by gravitational radiation.

3 figures. To appear in Phys.Rev.D

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Cited by in corpus (9)

• Rotating Stars in Relativity
• Gravitational wave asteroseismology of fast rotating neutron stars with realistic equations of state
• A gravitational wave afterglow in binary neutron star mergers
• Equilibrium solutions of relativistic rotating stars with mixed poloidal and toroidal magnetic fields
• Oscillation modes of rapidly rotating neutron stars in scalar-tensor theories of gravity
• Dynamics of Fast Rotating Neutron Stars: An Approach in the Hilbert Gauge
• Constraining nuclear parameters using Gravitational waves from f-mode Oscillations in Neutron Stars
• Fast Rotating Neutron Stars: Oscillations and Instabilities
• Prospect of unraveling the first-order phase transition in neutron stars with $f$ and $p_1$ modes