Secular stability of rotating stars

Conference · Sun Jan 01 04:00:00 EST 1984

OSTI ID:7010727

Imamura, J N; Friedman, J L; Durisen, R H

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

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
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