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Reviews in Modern Astronomy pp 145–156Cite as

Turbulence in the Solar Wind

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Part of the book series: Reviews in Modern Astronomy ((MOD.ASTRONOMY,volume 4))

Abstract

The solar wind is, apparently, a turbulent medium permeated by fluctuations on a broad range of scales characterizing the plasma as a fluid and kinetic entity. Here we briefly review some recent developments and observations on MHD fluctuations in the frequency range between some 10−6 and 10−2 Hz. Spectral analysis reveals that solar wind fluctuations represent ongoing turbulence, often with high Alfvénic correlations of coronal origin, which undergoes considerable spatial and spectral evolution in the radially expanding wind and is coupled to large-scale plasma structures and magnetic field inhomogeneities. Theoretical attempts to model the transport of magnetohydrodynamic fluctuations are discussed. Finally, the dissipation of turbulence and concurrent heating of the wind are addressed.

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Author information

Authors and Affiliations

  1. Max-Planck-Institut für Aeronomie, Postfach 20, W-3411, Katlenburg-Lindau, Fed. Rep. of Germany

    E. Marsch

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  1. E. Marsch
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Editor information

Editors and Affiliations

  1. Landessternwarte, Königstuhl, W-6900, Heidelberg 1, Fed. Rep. of Germany

    Gerhard Klare

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© 1991 Springer-Verlag Berlin Heidelberg

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Marsch, E. (1991). Turbulence in the Solar Wind. In: Klare, G. (eds) Reviews in Modern Astronomy. Reviews in Modern Astronomy, vol 4. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-76750-0_10

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  • DOI: https://doi.org/10.1007/978-3-642-76750-0_10

  • Publisher Name: Springer, Berlin, Heidelberg

  • Print ISBN: 978-3-642-76752-4

  • Online ISBN: 978-3-642-76750-0

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