Viscosity driven instability in rotating relativistic stars

Abstract

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 an m=2 perturbationin 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 the compactness of the star and takes values around 0.13 ~ 0.16, which differ slightly from that of Newtonian incompressible stars (~ 0.14). For differentially rotating stars, the critical value of T/W is found to span the range 0.17 - 0.25. This is significantly larger than the uniformly rotating case with the same compactness of the star. Finally we discuss a possibility of detecting gravitational waves from viscosity driven instability with ground-based interferometers.

v1: 14 pages with 10 figures, revtex4.cls. Submitted to Physical Review D; v2: Minor correction to the central enthalpy and typos, 13 pages with 10 figures, revtex4.cls. Physical Review D (2006) in press; v3: Published version, 13 pages with 10 figures, revtex4.cls. Physical Review D (2006) 084006

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Cited by in corpus (8)

• Spectral Methods for Numerical Relativity
• Quasi-equilibrium models for triaxially deformed rotating compact stars
• On the well-posedness of relativistic viscous fluids
• Do triaxial supramassive compact stars exist?
• On the well-posedness of relativistic viscous fluids with non-zero vorticity
• Gravitational wave content and stability of uniformly, rotating, triaxial neutron stars in general relativity
• Numerical simulations of oscillating and differentially rotating neutron stars
• Triaxial instabilities in rapidly rotating Neutron Stars