Instability of a nonlinearly pulsating model stellar system. III - Volume perturbations superposed on a nonequilibrium Einstein sphere

Details Instability of a nonlinearly pulsating model stellar system. III - Volume perturbations superposed on a nonequilibrium Einstein sphere Instability of a nonlinearly pulsating model stellar system. III - Volume perturbations superposed on a nonequilibrium Einstein sphere

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985azh....62..506n&link_type=abstract

(Astronomicheskii Zhurnal, vol. 62, May-June 1985, p. 506-517) Soviet Astronomy (ISSN 0038-5301), vol. 29, May-June 1985, p. 293

Astronomy and Astrophysics

Astronomy

3

Astronomical Models, Einstein Equations, Galactic Evolution, Perturbation Theory, Star Clusters, Stellar Oscillations, Stellar Systems, Barred Galaxies, Jeans Theory, Nonequilibrium Conditions, Nonlinear Systems, Spheres, Stellar Evolution, Stellar Motions, Systems Stability

Scientific paper

The author's nonlinearly pulsating model with elliptic star orbits, based on an equilibrium Einstein model sphere (Paper I), is tested for stability against volume perturbations. The corresponding complete and exact dispersion relation is derived. A thorough analysis is made of the global m = 1, N = 3 harmonic, representing 'egg shaped' perturbations. In the nonsteady model, anisotropic instability will set in beginning when the radial pulsations and the transverse motions have an energy ratio Delta asterisk = 0.826. At this critical state the ratio of the maximum and minimum radii will be 11.2, half that found for barlike (ellipsoidal) surface-type perturbations. When the pulsation amplitude reaches its maximum value, the configuration will experience power-law Jeans-type instability. The model also has a narrow island of instability against the barlike disturbances considered in Paper I, apparently a resonance stemming from the model's nonequilibrium character.

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