VLF Waves in the Foreshock

R. J. Strangeway* and G. W. Crawford**

*Institute of Geophysics and Planetary Physics,
University of California at Los Angeles

**Radio Atmosphere Science Center
Kyoto University at Kyoko 611, Japan
Now at SRI International, Menlo Park, California 94025, U. S. A.


Adv. Space Res., vol 15, (8/9)29-(8/9)42, 1995
Copyright 1995 by COSPAR


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Figure Captions

Fig. 1. a) Phase space contours of the incident and reflected solar wind electron population, in the de Hoffman-Teller frame (after /15/). b) Reflected electron flux and energy as a function of bn (after /15/).

Fig. 2. Foreshock electron distributions (after /18/). The left panels (a) show theoretical phase space density contours, together with the reduced distribution function. The right panels (b) show the same phase distributions, but sampled in a manner similar to a particle instrument. In this case the reduced distribution functions (solid curves) are compared with actual observations (dotted curves).

Fig. 3. Foreshock coordinate system at Venus (after /20, 21/).

Fig. 4. Example of VLF emissions observed in the foreshock at Venus (after /20, 21/).

Fig. 5.VLF map of the Venus foreshock for nominal Parker spiral (after /20/).

Fig. 6.VLF map of the Venus foreshock for perpendicular IMF (after /20/).

Fig. 7.Example of down-shifted plasma oscillations observed in the terrestrial electron foreshock (after /35/).

Fig. 8. Solutions of the beam-plasma dispersion relation. The left panel shows growth rate versus frequency for different beam velocities. The right panel shows the frequency at which maximum growth occurs as a function of beam velocity for different beam temperatures (after /35/).


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