On parametric instability and MHD turbulence evolution in high-latitude heliosphere

Details On parametric instability and MHD turbulence evolution in high-latitude heliosphere On parametric instability and MHD turbulence evolution in high-latitude heliosphere

Mar 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.477..313b&link_type=abstract

In: Proceedings of the Second Solar Cycle and Space Weather Euroconference, 24 - 29 September 2001, Vico Equense, Italy. Editor:

Physics

1

Alfvenic Turbulence, Solar Wind

Scientific paper

Solar wind plasma and magnetic field measurements by Ulysses during its first solar orbit have allowed extensive investigations on the radial evolution of Alfvénic fluctuations in the polar solar wind 1 to 5 AU. A noteworthy result is that the radial regime changes with heliocentric distance. Up to about 2.5 AU the dominant outward propagating fluctuations decrease more rapidly than the inward ones. Farther out, however, a steepening of the gradient for inward fluctuations is observed. A state is quickly reached where both kinds of fluctuation decline at approximately the same rate in the presence of a surviving excess of outward fluctuation energy. Recent simulations of the nonlinear development of the parametric instability for non-monochromatic Alfvén waves have given results that closely resemble the observed polar turbulence behavior. Thus, it would seem that when the generation from velocity gradients becomes negligible, as in the case of polar wind, the parametric instability can play a major role in driving turbulence evolution.

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