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

Paolo Pani1,*, Emanuele Berti2,3,†, Vitor Cardoso2,4,‡, Yanbei Chen3,§, and Richard Norte3,∥

  • 1Dipartimento di Fisica, Università di Cagliari, and INFN sezione di Cagliari, Cittadella Universitaria 09042 Monserrato, Italy
  • 2Department of Physics and Astronomy, The University of Mississippi, University, Mississippi 38677-1848, USA
  • 3Theoretical Astrophysics 350-17, California Institute of Technology, Pasadena, California 91125, USA
  • 4Centro Multidisciplinar de Astrofísica - CENTRA, Departamento de Física, Instituto Superior Técnico, Av. Rovisco Pais 1, 1049-001 Lisboa, Portugal

  • *paolo.pani@ca.infn.it Currently at Centro Multidisciplinar de Astrofísica - CENTRA, Departamento de Física, Instituto Superior Técnico, Av. Rovisco Pais 1, 1049-001 Lisboa, Portugal
  • †berti@phy.olemiss.edu
  • ‡vitor.cardoso@ist.utl.pt
  • §yanbei@tapir.caltech.edu
  • ∥norte@caltech.edu
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Phys. Rev. D 80, 124047 – Published 30 December, 2009

DOI: https://doi.org/10.1103/PhysRevD.80.124047

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 ultracompact objects. In order to set up a straw-man ultracompact 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 quasinormal modes 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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See Also

Gravitational wave signatures of the absence of an event horizon. II. Extreme mass ratio inspirals in the spacetime of a thin-shell gravastar

Paolo Pani, Emanuele Berti, Vitor Cardoso, Yanbei Chen, and Richard Norte
Phys. Rev. D 81, 084011 (2010)

Article Text

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Phys. Rev. D 80, 124047– Published 30 December, 2009
  • Received 1 September 2009

© 2009 American Physical Society

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