Nonlinear evolution of interplanetary Alfvénic fluctuations with convected structures
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Ghosh, S., Siregar, E., Roberts, D. A., and Goldstein, M. L. (1996), Simulation of high-frequency solar wind power spectra using Hall magnetohydrodynamics, J. Geophys. Res., 101(A2), 2493–2504, doi:10.1029/95JA03201.
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This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Abstract
At least at solar minimum, many regions in slow solar wind near the heliospheric current sheet have very low Alfvénicity. Motivated by recent suggestions that the interaction of the waves with the observed striated density, temperature, and magnetic field structures in the low Alfvénicity regions causes the decay of outward dominance, we have used two- and three-dimensional MHD codes to simulate such situations to determine the evolution. We find that outward propagating waves in the presence of structures become only slightly less Alfvénic (unlike observations), and that what were initially parallel propagating waves fairly rapidly become nearly isotropic with a self-similar spectrum typical of turbulence (similar to observations). These simulations suggest that the low Aflvénicty regions must arise from some other cause, such as “microstreams” that are eradicated as they decrease the Alfvénic correlations.