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MHD Turbulence in the Solar Wind

  • Chapter
Physics of the Inner Heliosphere II

Part of the book series: Physics and Chemistry in Space ((SPACE,volume 21))

Abstract

From the very beginning of in situ observations of the solar wind it was realized that the interplanetary medium by all appearances was usually not quiet but rather turbulent and visibly permeated by sizable fluctuations of the plasma flow velocity and density and of the magnetic field. Fluctuations occurred on all observed spatial and temporal scales, extending from the vast dimensions of the inner heliosphere and the corresponding solar wind transit time, or from the solar rotation period, down to the minute kinetic scales associated with the particles’ gyromotion, where the dissipation was assumed finally to occur. The observational studies often revealed random and nonreproducible behavior of solar wind parameters as a function of time, thus indicating properties typical of a turbulent magnetofluid. The measured fractional variances of the magnetic field components, when normalized to the mean intensity, turned out to be large, suggesting the importance of nonhnear processes that couple a large number of degrees of freedom and turbulent “eddies” of disparate scales.

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Marsch, E. (1991). MHD Turbulence in the Solar Wind. In: Schwenn, R., Marsch, E. (eds) Physics of the Inner Heliosphere II. Physics and Chemistry in Space, vol 21. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-75364-0_5

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