By A. J. Hundhausen
Little greater than ten years have handed on account that spaceprobe-borne tools con clusively confirmed the lifestyles of the sunlight wind. those observations con firmed the elemental validity of a theoretical version, first proposed by way of E. N. Parker, predicting a continuing, quick growth of the sun corona. the following decade has noticeable an important progress in either the breadth and class of sun wind observations; the houses of the interplanetary plasma close to the orbit of the earth at the moment are identified in nice element. the speculation of the coronal ex pansion has additionally been hugely refilled either within the feel of together with extra actual strategies, and of treating extra lifelike (time-dependent and non spheri cally-symmetric) coronal boundary stipulations. the current quantity is an try to synthesize the sun wind observations and coronal growth types from this decade of quick improvement. the final word objective is, in fact, the translation of saw sunlight wind phenomena because the results of easy actual strategies happening within the coronal and interplanetary plasma and because the traditional manifestations of sunlight homes and constructions. This technique implies an emphasis upon the "large-scale" gains printed by way of the observations. It calls for large use of the thoughts and techniques of fluid mechanics.
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Additional resources for Coronal Expansion and Solar Wind
5, reveals a wealth of variations in physical properties on a wide range of time scales. The presence of these variations shows that the coronal expansion is far more complicated than the steady, structureless flow assumed by Parker in his attempt to understand the basic characteristics of the interplanetary medium. 1J of 1963. "We will be surprised if future observation does not indicate a The Classification of Solar Wind Phenomena 21 restatement of many of the small scale effects that are assumed, and we will be very surprised indeed if observation does not discover a number of complications that have been entirely unanticipated in the present writing....
Large variations do occur on the basic time scale of the coronal expansion. 2 95% Confidence Level O r-----------------------------------------~ o 30 120 Fig. 6] A further result of the variation analysis of Gosling and Bame is displayed in Fig. 5. Here O"~ is shown for time lags between 0 and 130 h. The deviation from the best-fit line has been computed separately for two classes of observations; 0"2L is computed only from "low-speed" solar wind, defmed by u(t o)<404kmsec-t, while 0"2H is computed only from "high-speed" solar wind, defined by u(to) > 404 km sec -1.
The resulting comparisons may lead to a valid interpretation of basic physical processes affecting the coronal expansion. They may also be confused by the unidentified effects of the temporal variations and spatial structures that we have seen to be extremely common in the real solar wind. 3 The Physical Properties of Low-Speed Solar Wind Pursuit of our qualified identification of low-speed solar wind as the structureless coronal expansion leads to several practical difficulties. , with which the theoretical models will be compared.