Plasma instabilities of trapped particles in solar magnetic fields

Details Plasma instabilities of trapped particles in solar magnetic fields Plasma instabilities of trapped particles in solar magnetic fields

May 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978a%26a....65..369b&link_type=abstract

Astronomy and Astrophysics, vol. 65, no. 3, May 1978, p. 369-384. Research supported by the Schweizerischer Nationalfonds zuer

Astronomy and Astrophysics

Astrophysics

28

Electrostatic Waves, Magnetically Trapped Particles, Magnetohydrodynamic Stability, Solar Magnetic Field, Solar Radio Bursts, Whistlers, Electric Corona, Electron Precipitation, Fine Structure, Particle Emission, Type 4 Bursts, Wave Dispersion

Scientific paper

Electromagnetic whistler and electrostatic (hydrodynamic) instabilities in a magnetized plasma are studied with reference to the loss-cone velocity distribution function of particles. In the electrostatic case, maximum growth rate and marginal stability are considered. For whistler waves, the area of instability is spatially limited by the extent of the loss-cone distribution. Thus, while the growth rate for the whistler instability peaks at the feet of the arches, the electrostatic instability is restricted to zones near places where the upper hybrid frequency of the background particles is an integer multiple of the electron cyclotron frequency. It is noted that the electrostatic instability will become saturated, i.e., in a state of quasi-equilibrium, with the losses of untrapped particles. Whistler growth, however, is limited by field curvature in a twisted magnetic field, or by refraction.

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