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Probing the solar wind acceleration region using spectroscopic techniques

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Abstract

Measurements of the intensities and profiles of UV and EUV spectral lines can provide a powerful tool for probing the physical conditions in the solar corona out to 8 R ⊙ and beyond. We discuss here how measurements of spectral line radiation in conjunction with measurements of the white light K-corona can provide information on electron, proton and ion temperatures and velocity distribution functions; densities; chemical abundances and mass flow velocities. Because of the fundamental importance of such information, we provide a comprehensive review of the formation of coronal resonance line radiation, with particular emphasis on the H i Lα line, and discuss observational considerations such as requirements for rejection of stray light and effects of emission from the geocorona and interplanetary dust. Finally, we summarize some results of coronal H i Lα and white light observations acquired on sounding rocket flights.

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Authors and Affiliations

  1. Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass., USA

    George L. Withbroe, John L. Kohl & Heinz Weiser

  2. High Altitude Observatory, Boulder, Colo., USA

    Richard H. Munro

Authors
  1. George L. Withbroe
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  2. John L. Kohl
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  3. Heinz Weiser
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  4. Richard H. Munro
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Withbroe, G.L., Kohl, J.L., Weiser, H. et al. Probing the solar wind acceleration region using spectroscopic techniques. Space Sci Rev 33, 17–52 (1982). https://doi.org/10.1007/BF00213247

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