Interplanetary transport of solar electrons and protons - Effect of dissipative processes in the magnetic field power spectrum

Details Interplanetary transport of solar electrons and protons - Effect of dissipative processes in the magnetic field power spectrum Interplanetary transport of solar electrons and protons - Effect of dissipative processes in the magnetic field power spectrum

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....9813261a&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. A8, p. 13,261-13,280.

Physics

26

Interplanetary Medium, Ion Cyclotron Radiation, Particle Motion, Solar Electrons, Solar Protons, Mathematical Models, Particle Trajectories, Wave Dispersion, Whistlers

Scientific paper

A model of an observed interplanetary turbulence spectrum is developed which requires the dissipation range to be constituted by parallel dispersive whistler, electron, and ion cyclotron waves in a warm plasma. The dispersion relation of heavily thermally affected ion cyclotron waves needed in this model is calculated for the first time. The model is fitted to the turbulence spectrum measured on June 7, 1980 by ISEE 3 (ICE). The derived model parameters are used in a quasi-linear calculation of both proton and electron mean free paths. As a first step resonance broadening due to wave damping is neglected. The results are compared with typical empirical proton mean free paths and with electron mean free paths obtained from fits to electron intensity and anisotropy profiles observed simultaneously by the same satellite. In both cases the theoretical values seem to be systematically larger than the empirical ones. Thus scattering enhancements by nonlinear or thermal resonance broadening or oblique waves now bear the hope to remove the discrepancy between theory and observation.

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