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Interpretation of Observed Relations between Solar Wind Characteristics and Effects at Ionospheric Altitudes

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High-Latitude Space Plasma Physics

Part of the book series: Nobel Foundation Symposia Published by Plenum ((NOFS,volume 54))

Abstract

Convection of plasma and magnetic flux within the Earth’s magnetosphere, driven by coupling to the external flow of the solar wind, is the single most important factor governing the structure and dynamics of magnetospheric charged particle populations and electromagnetic fields. The magnetospheric flow is communicated along equipotential magnetic field lines to the ionosphere, where flows and electric currents are driven which dominate at high latitudes, above the plasmasphere. This flow is important in the transport and distribution of high latitude ionization, and the Joule heating which is associated with it can form an important source of energy. At the same time, particle precipitation into the atmosphere from the spatially structured magnetospheric plasma populations set up by convection contributes both to the ionospheric ionization and energy budgets.

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  1. Blackett Laboratory, Imperial College, London, SW7 2BZ, UK

    Stanley W. H. Cowley

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  1. Kiruna Geophysical Institute, Kiruna, Sweden

    Bengt Hultqvist

  2. EISCAT Scientific Association, Kiruna, Sweden

    Tor Hagfors

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Cowley, S.W.H. (1983). Interpretation of Observed Relations between Solar Wind Characteristics and Effects at Ionospheric Altitudes. In: Hultqvist, B., Hagfors, T. (eds) High-Latitude Space Plasma Physics. Nobel Foundation Symposia Published by Plenum, vol 54. Springer, Boston, MA. https://doi.org/10.1007/978-1-4613-3652-5_13

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