Evolution of Turbulent Magnetic Fluctuation Power with Heliospheric Distance
G. P. Zank, W. H. Matthaeus and C. W. Smith
Journal of Geophysical Research, A101, 17,093-17,107 (1996)
On the basis of transport theories appropriate to a radially expanding solar wind, new results for the evolution of the energy density in solar wind fluctuations at MHD scales are derived. The models, which represent a departure from the well-known WKB description, include the effects of ``mixing'', driving the stream-stream interactions (compression and shear) and interstellar pick-up ions as well as non-isotropic MHD turbulence. Magnetometer data from Voyager 1 and 2 and Pioneer 11 are compared to the turbulence-based models and close agreement is found between theory and data for a reasonable choice of parameters.
Return to Charles W. Smith's Publication Page
Return to Charles W. Smith Home Page