Viscosity driven instability in rotating relativistic stars

Motoyuki Saijo, Eric Gourgoulhon

Research output: Contribution to journalArticle

12 Citations (Scopus)

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 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 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.

Original languageEnglish
Article number084006
JournalPhysical Review D - Particles, Fields, Gravitation and Cosmology
Volume74
Issue number8
DOIs
Publication statusPublished - 2006
Externally publishedYes

Fingerprint

Star
Viscosity
Rotating
viscosity
stars
void ratio
Compactness
gravitational binding energy
Binding Energy
Gravitational Waves
Kinetic energy
Equation of State
Interferometer
gravitational waves
Critical value
stiffness
Stiffness
equations of state
interferometers
kinetic energy

ASJC Scopus subject areas

  • Physics and Astronomy(all)
  • Nuclear and High Energy Physics
  • Mathematical Physics

Cite this

Viscosity driven instability in rotating relativistic stars. / Saijo, Motoyuki; Gourgoulhon, Eric.

In: Physical Review D - Particles, Fields, Gravitation and Cosmology, Vol. 74, No. 8, 084006, 2006.

Research output: Contribution to journalArticle

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