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Microscopic structure of the solar wind

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Abstract

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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  1. Space Sciences Laboratory, TRW Systems Group, Redondo Beach, Calif., USA

    Frederick L. Scarf

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  1. Frederick L. Scarf
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Scarf, F.L. Microscopic structure of the solar wind. Space Sci Rev 11, 234–270 (1970). https://doi.org/10.1007/BF00241523

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  • DOI: https://doi.org/10.1007/BF00241523

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