Multicomponent theory of buoyancy instabilities in magnetized astrophysical plasmas: MHD analysis revisited

Details Multicomponent theory of buoyancy instabilities in magnetized astrophysical plasmas: MHD analysis revisited Multicomponent theory of buoyancy instabilities in magnetized astrophysical plasmas: MHD analysis revisited

2010-02-28

arxiv.org/abs/1003.0204v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

25 pages, submitted to Astrophysical Journal

Scientific paper

We develop a theory of buoyancy instabilities of the electron-ion plasma with the heat flux based on not the MHD equations, but using the multicomponent plasma approach. We investigate a geometry in which the background magnetic field, gravity, and stratification are directed along one axis. No simplifications usual for the MHD-approach in studying these instabilities are used. The background electron thermal flux and collisions between electrons and ions are included. We derive the simple dispersion relation, which shows that the thermal flux perturbation generally stabilizes an instability. There is a narrow region of the temperature gradient, where an instability is possible. This result contradicts to a conclusion obtained in the MHD-approach. We show that the reason of this contradiction is the simplified assumptions used in the MHD analysis of buoyancy instabilities and the role of the longitudinal electric field perturbation, which is not captured by the MHD equations. Our dispersion relation also shows that a medium with the electron thermal flux can be unstable, if the temperature gradient of ions and electrons have the opposite signs. The results obtained can be applied to ICM and clusters of galaxies.

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