Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ap%26ss.308..481s&link_type=abstract
Astrophysics and Space Science, Volume 308, Issue 1-4, pp. 481-485
Astronomy and Astrophysics
Astrophysics
Scientific paper
We investigate the instability driven by viscosity in rotating relativistic stars by means of an iterative approach. We focus on polytropic rotating equilibrium stars and impose an m=2 perturbation in the lapse. We vary both the stiffness of the equation of state and the compactness of the star to study these factors on the critical value T/W for the instability. For a rigidly rotating star, the criterion T/W, where T is the rotational kinetic energy and W the gravitational binding energy, mainly depends on the compactness of the star and takes values around 0.13 0.16, which slightly differ 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. The value is significantly larger than in the rigidly rotating case with the same compactness of the star. Finally we discuss the possibility of detecting gravitational waves from viscosity-driven instabilities using ground-based interferometers.
Gourgoulhon Eric
Saijo Motoyuki
No associations
LandOfFree
Instabilities in rotating relativistic stars driven by viscosity does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Instabilities in rotating relativistic stars driven by viscosity, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Instabilities in rotating relativistic stars driven by viscosity will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1682471