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Coronal Expansion and Solar Wind

  • Book
  • © 1972

Overview

Authors:
  1. A. J. Hundhausen

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

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Part of the book series: Physics and Chemistry in Space (SPACE, volume 5)

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Table of contents (7 chapters)

  1. Front Matter

    Pages I-XII
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  2. History and Background

    • A. J. Hundhausen
    Pages 1-19

  3. The Identification and Classification of Some Important Solar Wind Phenomena

    • A. J. Hundhausen
    Pages 20-35

  4. The Dynamics of a Structureless Coronal Expansion

    • A. J. Hundhausen
    Pages 36-93

  5. Chemical Composition of the Expanding Coronal and Interplanetary Plasma

    • A. J. Hundhausen
    Pages 94-120

  6. High-Speed Plasma Streams and Magnetic Sectors

    • A. J. Hundhausen
    Pages 121-168

  7. Flare-Produced Interplanetary Shock Waves

    • A. J. Hundhausen
    Pages 169-210

  8. Concluding Remarks

    • A. J. Hundhausen
    Pages 211-215

  9. Back Matter

    Pages 216-238
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Keywords

About this book

Little more than ten years have passed since spaceprobe-borne instruments conยญ clusively demonstrated the existence of the solar wind. These observations conยญ firmed the basic validity of a theoretical model, first proposed by E. N. Parker, predicting a continuous, rapid expansion of the solar corona. The subsequent decade has seen a tremendous growth in both the breadth and sophistication of solar wind observations; the properties of the interplanetary plasma near the orbit of the earth are now known in great detail. The theory of the coronal exยญ pansion has also been highly refilled both in the sense of including additional physical processes, and of treating more realistic (time-dependent and non spheriยญ cally-symmetric) coronal boundary conditions. The present volume is an attempt to synthesize the solar wind observations and coronal expansion models from this decade of rapid development. The ultimate goal is, of course, the interpretation of observed solar wind phenomena as the effects of basic physical processes occurring in the coronal and interplanetary plasma and as the natural manifestations of solar properties and structures. This approach implies an emphasis upon the "large-scale" features revealed by the observations. It requires extensive use of the concepts and methods of fluid mechanics.

Authors and Affiliations

  • High Altitude Observatory, National Center for Atmospheric Research, Boulder, USA

    A. J. Hundhausen

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