Titlebook: Coronal Expansion and Solar Wind; A. J. Hundhausen Book 1972 Springer-Verlag Berlin · Heidelberg 1972 Korona (Astron.).Orbit.Scale.Sonnenw

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Bulk growth of widegap II–VI single crystalsures and processes, has led to the neglect of several interesting and important areas of solar wind research. Some mention of such areas, along with recent reviews and key works that will serve to guide the reader interested in their exploration, is in order. Introductory treatments of many of these

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Physics and Chemistry in Spacehttp://image.papertrans.cn/c/image/238290.jpg

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The Identification and Classification of Some Important Solar Wind Phenomena, This era saw development of the basic concept of the solar wind as well as a model of its origin in the continuous expansion of the solar corona. Observations of a continuous supersonic flow of plasma and a magnetic field configuration fitting the expected pattern by the first spacecraft to probe i

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The Dynamics of a Structureless Coronal Expansion,y discussion of the physics of the interplanetary plasma. We have already seen that the models of Parker, based on the assumption of steady, spherically-symmetric fluid motion, correctly predicted the basic characteristics of the solar wind. The adoption of this same simplifying assumption in the fo

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High-Speed Plasma Streams and Magnetic Sectors,al solar wind. Mere inspection of solar wind data reveals large variations on a time scale of several days, comparable to the basic scale time of the overall coronal expansion (and thus indicative of phenomena in Class 2 of the classification scheme developed in Chapter II). Autocorrelation analysis

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Flare-Produced Interplanetary Shock Waves,l ejected by the flare. Consider a volume of this material, presumably plasma from the chromosphere or low corona, moving rapidly outward into a slower ambient solar wind (such as already shown in Fig. 5.9). Fig. 6.1 shows a hypothetical cross section (in the solar equatorial plane) of the resulting

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