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The dynamics of astrophysical plasmas plays an increasingly important role in many areas of astrophysics. The solar wind or interplanetary medium is unique in providing a nearby, relatively accessible laboratory in which in situ observa tions of many astrophysical plasma phenomena can be carried out. Direct obser vations from spacecraft and indirect observations of phenomena from the Earth's surface are both used with effect in studying this phenomenon. The over all gross features of the solar wind are relatively well understood and have been covered thoroughly in a number of recent review articles (see, e.g., Dessler 1967, Lust 1967, Axford 1968, Ness 1968, Parker 1969, Hundhausen 1968, 1970, Holzer & Axford 1970, and Wolfe 1972). Table 1 provides a brief summary of nominal values of some of the important parameters of the plasma. In the last few years, as better models and more detailed observations have become available, it has become clear that fluctuations and waves are an essential aspect of the solar wind. Indeed, it is now generally accepted that a detailed understanding of even the average properties of the interplanetary plasma depends on an understanding of fluctuations. One may infer that this is generally true for
Annual Review of Astronomy and Astrophysics – Annual Reviews
Published: Sep 1, 1973
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