Nonlinear r-Modes in Rapidly Rotating Relativistic Stars

N. Stergioulas and José A. Font
Phys. Rev. Lett. 86, 1148 – Published 12 February 2001
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Abstract

The r-mode instability in rotating relativistic stars has been shown recently to have important astrophysical implications, provided that r-modes are not saturated at low amplitudes by nonlinear effects or by dissipative mechanisms. Here, we present the first study of nonlinear r-modes in isentropic, rapidly rotating relativistic stars, via 3D general-relativistic hydrodynamical evolutions. We find that (1) on dynamical time scales, there is no strong nonlinear coupling of r-modes to other modes at amplitudes of order one—the maximum r-mode amplitude is of order unity. (2) r-modes and inertial modes in isentropic stars are predominantly discrete modes. (3) The kinematical drift associated with r-modes appears to be present in our simulations, but confirmation requires more precise initial data.

  • Received 31 July 2000

DOI:https://doi.org/10.1103/PhysRevLett.86.1148

©2001 American Physical Society

Authors & Affiliations

N. Stergioulas1 and José A. Font2

  • 1Department of Physics, Aristotle University of Thessaloniki, Thessaloniki 54006, Greece
  • 2Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, D-85740 Garching, Germany

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Issue

Vol. 86, Iss. 7 — 12 February 2001

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