Secular stability of rotating stars
In this work, we calculate the secular stability limits of rotating polytropes to nonaxisymmetric perturbations of low m. We consider polytropic indices ranging from 1 to 3 and several angular momentum distributions. Results are most conveniently presented in terms of the t-parameter, defined as the ratio of the rotational kinetic energy to the absolute value of the gravitational energy of the fluid. Previous work on polytropes considered only the m = 2 mode, which is unstable for values of the t-parameter greater than 0.14 +- 0.01 for the n values n = 1.5 and 3 and the angular momentum distributions tested (see Durisen and Imamura 1981). The GRR secular stability limit of the m = 2 mode for the Maclaurin spheroids (n = O) was determined by Chandrasekhar (1970). GRR stability limits of higher m modes for the Maclaurin spheroids were located approximately by Comins (1979a,b) and more precisely by Friedman (1983).
- Research Organization:
- Los Alamos National Lab., NM (USA); Wisconsin Univ., Milwaukee (USA); Indiana Univ., Bloomington (USA)
- DOE Contract Number:
- W-7405-ENG-36
- OSTI ID:
- 7010727
- Report Number(s):
- LA-UR-84-2088; CONF-8406151-1; ON: DE84014011
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ANGULAR MOMENTUM
DATA
FUNCTIONS
INFORMATION
LAGRANGIAN FUNCTION
MASS
MATHEMATICAL MODELS
MOTION
NUMERICAL DATA
ROTATION
STABILITY
STAR MODELS
THEORETICAL DATA