Gravitational Waves from Rotating Proto-Neutron Stars

Details Gravitational Waves from Rotating Proto-Neutron Stars Gravitational Waves from Rotating Proto-Neutron Stars

2004-09-24

arxiv.org/abs/astro-ph/0409578v1

Class.Quant.Grav.21:S515-S519,2004

Astronomy and Astrophysics

Astrophysics

5 pages, proceedings of the 5th Edoardo Amaldi Conference On Gravitational Waves

Scientific paper

10.1088/0264-9381/21/5/019

We study the effects of rotation on the quasi normal modes (QNMs) of a newly born proto neutron star (PNS) at different evolutionary stages, until it becomes a cold neutron star (NS). We use the Cowling approximation, neglecting spacetime perturbations, and consider different models of evolving PNS. The frequencies of the modes of a PNS are considerably lower than those of a cold NS, and are further lowered by rotation; consequently, if QNMs were excited in a sufficiently energetic process, they would radiate waves that could be more easily detectable by resonant-mass and interferometric detectors than those emitted by a cold NS. We find that for high rotation rates, some of the g-modes become unstable via the CFS instability; however, this instability is likely to be suppressed by competing mechanisms before emitting a significant amount of gravitational waves.

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