Authors: Paolo Pani, Emanuele Berti, Vitor Cardoso, Yanbei Chen, Richard Norte
Date: 1 Sep 2009
Abstract: 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 the nonrotating thin-shell gravastar model first proposed by Mazur and Mottola, which has a Schwarzschild exterior, a de Sitter interior and an infinitely thin shell with finite surface energy and 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 gravastar, 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 its 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 is superluminal.
© M. Vallisneri 2012 — last modified on 2010/01/29
Tantum in modicis, quantum in maximis