Secular stability limits for rotating polytropic stars

Details Secular stability limits for rotating polytropic stars Secular stability limits for rotating polytropic stars

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...294..474i&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 294, July 15, 1985, p. 474-478. DOE-supported research.

Statistics

Computation

61

Gravitational Waves, Pulsars, Secular Variations, Stellar Oscillations, Stellar Rotation, Systems Stability, Angular Momentum, Compressibility Effects, Computational Astrophysics, Maclaurin Series, Polytropic Processes, Stellar Gravitation, Stellar Models, Variational Principles

Scientific paper

The Lagrangian variational principle is used to numerically locate the secular stability limits of rotating polytropes to nonaxisymmetric perturbations. It has been suggested that nonaxisymmetric modes, with exp(imφ) azimuthal dependence, set upper bounds on the rotation rate of compact stars when driven by gravitational radiation reaction. The results of this paper show that, in contrast to the m = 2 bar mode, the secular stability limits for modes with m > 2 are quite sensitive to the compressibility and angular momentum distribution of the polytrope.

Affiliated with

Also associated with

No associations

Rating

Secular stability limits for rotating polytropic stars 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 Secular stability limits for rotating polytropic stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Secular stability limits for rotating polytropic stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1231141