Coronal Expansion and Solar Wind by A. J. Hundhausen

By A. J. Hundhausen

Little greater than ten years have handed in view that spaceprobe-borne tools con­ clusively verified the lifestyles of the sunlight wind. those observations con­ firmed the elemental validity of a theoretical version, first proposed by means of E. N. Parker, predicting a continuing, speedy growth of the sun corona. the next decade has visible an immense development in either the breadth and class of sun wind observations; the homes 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 techniques, and of treating extra life like (time-dependent and non spheri­ cally-symmetric) coronal boundary stipulations. the current quantity is an try to synthesize the sun wind observations and coronal enlargement types from this decade of fast improvement. the last word aim is, in fact, the translation of saw sunlight wind phenomena because the results of easy actual tactics happening within the coronal and interplanetary plasma and because the traditional manifestations of sunlight houses and buildings. This process implies an emphasis upon the "large-scale" gains published by means of the observations. It calls for huge use of the suggestions and strategies of fluid mechanics.

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At short time lags, 0"2L < 0"2H' indicating that u(t o) and u(to + L) are more nearly equal at low solar wind speeds u(t o) than at high solar wind speeds. This is in agreement with the result shown in Fig. 2. However, at time lags near SOh, C2L;:::;0"2H;:::;C~. The variations on a 50-hour time scale are large even when attention is restricted to low solar wind speeds. Chapter III. 5 The standard deviations of the best-fit lines to u(t o + L) vs. 6], O"Kt; for observations with u(to)<404kmsec-1, O"EL; and for observations with u(t o»404kmsec-1, O"EH This analysis lends little support to the supposition that low-speed solar wind corresponds to a structureless coronal expansion.

Yet, in practice, only the Whang and Chang model (with Tocr- 2 / 5 at large r) can be so utilized. 14J. 2 reveals this to be a poor approximation near 1 AU in the observed solar wind. The solutions with Toc r- 4 / 3 at large r have not yet been published in sufficient detail to allow comparison with observations at a finite heliocentric position. Thus we must rely on the Whang and Chang model in the following discussions. This practical limitation is more serious than may be at first apparent. 26265, where re is the critical radius.

For extremely high densities, the subsonic models of Chamberlain become the valid solutions to the one-fluid equations. It might thus appear that three different types of "one-fluid" models are available for comparison with solar wind observations and with the other models to be described below. Yet, in practice, only the Whang and Chang model (with Tocr- 2 / 5 at large r) can be so utilized. 14J. 2 reveals this to be a poor approximation near 1 AU in the observed solar wind. The solutions with Toc r- 4 / 3 at large r have not yet been published in sufficient detail to allow comparison with observations at a finite heliocentric position.

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