HR: 0830h
AN: SH41B-0471    [PDF]
TI: Macroscopic Instability of the Ion Shell Distribution Function in the Divergent Solar Wind
AU: * Shevchenko, V I
EM: vshevchnko@ucsd.edu
AF: University of California, San Diego, 9500 Gilman Drive, La Jolla, CA 92093-0407 United States
AU: Galinsky, V L
EM: vit@ucsd.edu
AF: University of California, San Diego, 9500 Gilman Drive, La Jolla, CA 92093-0407 United States
AU: Sagdeev, R Z
AF: University of Maryland, Department of physics, College Park, College Park, MD 20742-3280 United States
AU: Winske, D
EM: winske@lanl.gov Dan Winske (winske@lanl.gov
AF: Los Alamos National laboratory, Los Alamos NATL LAB, Applied Theoretical Physiscs Division, Los Alamos, Los Alamos, NM 87545 United States
AB: As a result of cyclotron interaction with Alfven waves propagating from the sun, pitch angle diffusion of resonant particles takes place and shell-like distribution function of resonant ions (protons) is formed at each distance from the sun [V. Galinsky and V. Shevchenko, Phys. Rev. Lett., 85, 90, 2000]. Stability of the solar wind ion shell-like distribution function with respect to excitation of waves at larger distances is addressed. It is shown in linear approximation, that in case when the phase velocity of Alfven waves decreases with distance, ions with shell distribution excite outward propagating Alfven waves with smaller phase velocities when they advance to larger distances. The real problem, how the shell distribution, created at some distance from the sun, is changed due to interaction with Alfven fluctuations with smaller phase velocities at larger distances in the divergent solar wind, is studied in quasi-linear approximation and by numerical simulations.
DE: 2114 Energetic particles, heliospheric (7514)
DE: 2149 MHD waves and turbulence
DE: 2164 Solar wind plasma
DE: 7867 Wave/particle interactions
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting