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Dynamical instability of fluid spheres in the presence of a cosmological constant

C. G. Böhmer*

T. Harko†

  • The Erwin Schrödinger International Institute for Mathematical Physics, Boltzmanngasse 9, A-1090 Wien, Austria
  • Institut für Theoretische Physik, Technische Universität Wien, Wiedner Hauptstrasse 8-10, A-1040 Wien, Austria

  • Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong SAR, People’s Republic of China

  • *Electronic address: boehmer@hep.itp.tuwien.ac.at
  • †Electronic address: harko@hkucc.hku.hk
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Phys. Rev. D 71, 084026 – Published 25 April, 2005

DOI: https://doi.org/10.1103/PhysRevD.71.084026

Abstract

The equations describing the adiabatic, small radial oscillations of general relativistic stars are generalized to include the effects of a cosmological constant. The generalized eigenvalue equation for the normal modes is used to study the changes in the stability of the homogeneous sphere induced by the presence of the cosmological constant. The variation of the critical adiabatic index as a function of the central pressure is studied numerically for different trial functions. The presence of a large cosmological constant significantly increases the value of the critical adiabatic index. The dynamical stability condition of the homogeneous star in the Schwarzschild–de Sitter geometry is obtained and several bounds on the maximum allowable value for a cosmological constant are derived from stability considerations.

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Phys. Rev. D 71, 084026– Published 25 April, 2005
  • Received 18 January 2005

© 2005 American Physical Society

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