Gravitational wave signatures of the absence of an event horizon. I. Nonradial oscillations of a thin-shell gravastar

Details Gravitational wave signatures of the absence of an event horizon. I. Nonradial oscillations of a thin-shell gravastar Gravitational wave signatures of the absence of an event horizon. I. Nonradial oscillations of a thin-shell gravastar

2009-09-01

arxiv.org/abs/0909.0287v2

Phys.Rev.D80:124047,2009

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

19 pages, 8 figures. In press in Physical Review D. We found a new family of modes and improved the discussion of nonradial in

Scientific paper

10.1103/PhysRevD.80.124047

Gravitational waves from compact objects provide information about their structure, probing deep into strong-gravity regions. Here we illustrate how the presence or absence of an event horizon can produce qualitative differences in the gravitational waves emitted by ultra-compact objects. In order to set up a straw-man ultra-compact object with no event horizon, but which is otherwise almost identical to a black hole, we consider a nonrotating thin-shell model inspired by Mazur and Mottola's gravastar, which has a Schwarzschild exterior, a de Sitter interior and an infinitely thin shell with finite tension separating the two regions. As viewed from the external space-time, the shell can be located arbitrarily close to the Schwarzschild radius, so a gravastar might seem indistinguishable from a black hole when tests are only performed on its external metric. We study the linearized dynamics of the system, and in particular the junction conditions connecting internal and external gravitational perturbations. As a first application of the formalism we compute polar and axial oscillation modes of a thin-shell gravastar. We show that the quasinormal mode spectrum is completely different from that of a black hole, even in the limit when the surface redshift becomes infinite. Polar QNMs depend on the equation of state of matter on the shell and can be used to distinguish between different gravastar models. Our calculations suggest that low-compactness gravastars could be unstable when the sound speed on the shell vs/c>0.92.

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