Magnetic Fluctuations and Wave-Ion Interactions in the Solar Wind

Details Magnetic Fluctuations and Wave-Ion Interactions in the Solar Wind Magnetic Fluctuations and Wave-Ion Interactions in the Solar Wind

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsm22b..07g&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SM22B-07

Physics

2159 Plasma Waves And Turbulence, 2164 Solar Wind Plasma, 7827 Kinetic And Mhd Theory, 7867 Wave/Particle Interactions

Scientific paper

Large amplitude, long wavelength magnetic fluctuations (sometimes called "turbulence") are ubiquitously observed in the solar wind; by cascading to shorter wavelengths they may heat ions and induce ion/ion flows and ion anisotropies through wave-particle interactions. Thus this cascade drives the plasma away from thermal conditions, just as wave-particle scattering by kinetic instabilities acts to reduce anisotropies and ion/ion flows. If the turbulent fluctuation amplitudes are large enough, theory predicts that the alpha/proton relative flow in the solar wind should be subject to two constraints: an upper bound imposed by electromagnetic alpha/proton instabilities and a lower bound driven by the turbulent cascade. We have searched for these characteristic signatures of wave-particle interactions in the Ulysses/SWOOPS solar wind ion observations. The upper bound is trivially satisfied because the alpha/proton speed is typically well below the instability threshold. The lower bound is satisfied only in the high speed wind, presumably because that is where the magnetic fluctuations have sufficiently large amplitude to drive the alpha/proton flow.

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