Microscopic Structure of the Solar Wind

Details Microscopic Structure of the Solar Wind Microscopic Structure of the Solar Wind

Oct 1970

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1970ssrv...11..234s&link_type=abstract

Space Science Reviews, Volume 11, Issue 2-3, pp. 234-270

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19

Scientific paper

As the solar wind flows out from the coronal base the coulomb collision frequencies rapidly become small and particle-particle collisions can no longer maintain local statistical equilibrium. At 1 AU the particle distribution functions have important non-Maxwellian characteristics and the firehose instability, a cyclotron resonance whistler-mode instability, and several heat flux current instabilities should be operative. Superthermal particle populations also provide large wave levels, and other forms of enhanced plasma turbulence develop at shock fronts and discontinuities. This report contains a review of the theoretical concepts and a progress report on the experimental study of interplanetary wave-particle interactions.

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