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Acceleration of the solar wind

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Abstract

In this review, we discuss critically recent research on the acceleration of the solar wind, giving emphasis to high-speed solar wind streams emanating from solar coronal holes. We first explain why thermally driven wind models constrained by solar and interplanetary observations encounter substantial difficulties in explaining high speed streams. Then, through a general discussion of energy addition to the solar wind above the coronal base, we indicate a possible resolution of these difficulties. Finally, we consider the question of what role MHD waves might play in transporting energy through the solar atmosphere and depositing it in the solar wind, and we conclude by examining, in a simple way, the specific mechanism of solar wind acceleration by Alfvén waves and the related problem of accelerating massive stellar winds with Alfvén waves.

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Authors and Affiliations

  1. High Altitude Observatory, National Center for Atmospheric Research, 80307, Boulder, CO, USA

    Egil Leer, Thomas E. Holzer & Tor Flå

Authors
  1. Egil Leer
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  2. Thomas E. Holzer
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  3. Tor Flå
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On leave from the Auroral Observatory, Institute of Mathematical and Physical Sciences, University of Tromsø, N-9001 Tromsø, Norway.

The National Center for Atmospheric Research is sponsored by the National Science Foundation.

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Leer, E., Holzer, T.E. & Flå, T. Acceleration of the solar wind. Space Sci Rev 33, 161–200 (1982). https://doi.org/10.1007/BF00213253

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