Coronal Expansion and Solar Wind by A. J. Hundhausen

By A. J. Hundhausen

Little greater than ten years have handed due to the fact spaceprobe-borne tools con­ clusively tested the life of the sunlight wind. those observations con­ firmed the fundamental validity of a theoretical version, first proposed via E. N. Parker, predicting a continual, speedy enlargement of the sun corona. the following decade has obvious an enormous progress in either the breadth and class of sun wind observations; the houses of the interplanetary plasma close to the orbit of the earth are actually identified in nice element. the idea of the coronal ex­ pansion has additionally been hugely refilled either within the feel of together with extra actual methods, and of treating extra practical (time-dependent and non spheri­ cally-symmetric) coronal boundary stipulations. the current quantity is an try to synthesize the sunlight wind observations and coronal enlargement versions from this decade of speedy improvement. the last word objective is, in fact, the translation of saw sun wind phenomena because the results of uncomplicated actual strategies happening within the coronal and interplanetary plasma and because the usual manifestations of sunlight houses and buildings. This method implies an emphasis upon the "large-scale" positive aspects printed by means of the observations. It calls for wide use of the thoughts and strategies of fluid mechanics.

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I80° 8= -90 0 Fig. 23]. 23]. The angle ¢ is the solar ecliptic longitude of the observed vector field, while the angle () is the solar ecliptic latitude. The average field orientation was nearly (but not exactly) in the ecliptic plane, at ~ 45° from the radial direction (¢ = 0° or 180°). This is in basic agreement with the spiral field configuration of Fig. 4. The average field intensity determined on Imp 1 was 6 y, (where y = 10 - 5 gauss is the unit commonly used to specify the weak interplanetary field strength), a reasonable value on the basis of known solar magnetic fields.

Ec · ' ) 700 600 In Search of the Structureless Solar Wind 41 The best fit lines for the different time lags are shown in Fig. 3. As would be expected, the increased scatter at longer time lags produces best-fit lines with a decreasing slope, indicating that the autocorrelation coefficient AL becomes small at long time lags. Fig. 4 shows AL at lags between 0 and 120h. 3. Flow speeds observed with this temporal separation are only slightly related. 3-that the solar wind cannot be regarded as steady under average or typical conditions.

__ , \. .. N . ooPyi '. o.. '1. -t ' • " or ~ T , ',' , "' . or .. :". . r :,'1\. 1. •. ,......... ". ,,- ..... ,. ",' . r" .. :-~ Fig. 14]. The Cartesian components R, T, and N of the magnetic field (dots) and plasma velocity (horizontal lines) are defined in the text. The lowest frame shows the field magnitude and plasma density reflect the presence of tangential discontinuities, the interplanetary plasma consists of distinct, bounded plasma regimes (perhaps the "filaments" mentioned above) that retain their identity in the absence of instabilities and diffusion (processes that would be inhibited by the tangential nature of the field lines at boundary surfaces).

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