Collective instabilities of self-gravitating systems. II - Instabilities due to temperature anisotropy

Details Collective instabilities of self-gravitating systems. II - Instabilities due to temperature anisotropy Collective instabilities of self-gravitating systems. II - Instabilities due to temperature anisotropy

May 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975pthph..53.1348n&link_type=abstract

Progress of Theoretical Physics, vol. 53, May 1975, p. 1348-1359.

Physics

7

Astronomical Models, Galactic Rotation, Galactic Structure, Magnetohydrodynamic Stability, Stellar Systems, Wave Propagation, Anisotropic Media, Graphs (Charts), Gravitational Effects, Jeans Theory, Poisson Equation, Rotating Matter, Spiral Galaxies, Temperature Distribution, Vlasov Equations, Wave Dispersion

Scientific paper

The paper investigates theoretically the possibility that the Harris instability occurs in a rotating and self-gravitating system. The stability of the density wave which propagates obliquely to the rotational axis in an infinitely long self-gravitating and rotating cylinder is considered for two systems: (1) a collisionless stellar system with anisotropic velocity distribution and (2) a gaseous system with anisotropic pressure. It is found that in the collisionless stellar system, the Jeans instability will occur at the same time as the Harris instability, and the growth rate of the Jeans instability will always be the greater. For the gaseous system, the dispersion relation resembles that of magnetized plasma when an electron beam is injected. When propagation is perpendicular to the rotational axis, the Jeans mode is stabilized; under oblique or parallel propagation the Jeans instability occurs and under certain conditions, even the overstable mode appears. Application of these results to Galactic processes is briefly discussed.

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