Viscosity driven instability in rotating relativistic stars

  title={Viscosity driven instability in rotating relativistic stars},
  author={Motoyuki Saijo and E. Gourgoulhon},
  journal={Physical Review D},
We investigate the viscosity driven instability in rotating relativistic stars by means of an iterative approach. We focus on polytropic rotating equilibrium stars and impose a m=2 perturbation in the lapse. We vary both the stiffness of the equation of state and the compactness of the star to study those effects on the value of the threshold. For a uniformly rotating star, the criterion T/W, where T is the rotational kinetic energy and W is the gravitational binding energy, mainly depends on… 
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  • J. 460, 379
  • 1996
  • Astrophys. 331, 280
  • 1998
Classical Quantum Gravity 11
  • 1775
  • 1994
  • Rev. D 66, 044021
  • 2002
Classical Quantum Gravity 11
  • 443
  • 1994