Alfvénic Turbulence and Micro-Stream Structure in the Polar Solar Wind.

Details Alfvénic Turbulence and Micro-Stream Structure in the Polar Solar Wind. Alfvénic Turbulence and Micro-Stream Structure in the Polar Solar Wind.

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh53a1254l&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH53A-1254

Physics

7524 Magnetic Fields, 7839 Nonlinear Phenomena (4400, 6944), 7863 Turbulence (4490)

Scientific paper

We present 2D simulations of the interaction of an outwardly propagating Alfvén wave spectrum with micro-streams in the expanding solar wind. In previous work, we suggested that velocity shears in the developing solar wind could be responsible for the high-latitude polarity reversals observed by Ulysses. Here we carry out numerical experiments with more realistic initial conditions. We suggest that Alfvénic turbulence might play a role in determining the overall velocity differences in a stream- or jet- dominated early fast wind, surviving further out as the microstream structures, since turbulence may act as a sink for free energy in velocity shears. The magnitude of velocity shears at large distances from the sun is determined by the interplay of turbulent dissipation and magnetic tension. We compare simulation results with representative data from the Ulysses measurements.

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