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 lifestyles of the sunlight wind. those observations con­ firmed the fundamental validity of a theoretical version, first proposed via E. N. Parker, predicting a continuing, swift growth of the sunlight corona. the next decade has visible a major development in either the breadth and class of sunlight wind observations; the houses of the interplanetary plasma close to the orbit of the earth are actually recognized in nice element. the idea of the coronal ex­ pansion has additionally been hugely refilled either within the feel of together with extra actual approaches, and of treating extra sensible (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 fast improvement. the final word objective is, after all, the translation of saw sun wind phenomena because the results of simple actual tactics happening within the coronal and interplanetary plasma and because the common manifestations of sun houses and constructions. This strategy implies an emphasis upon the "large-scale" good points published via the observations. It calls for large use of the suggestions and strategies of fluid mechanics.

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By A. J. Hundhausen

Little greater than ten years have handed due to the fact spaceprobe-borne tools con­ clusively tested the lifestyles of the sunlight wind. those observations con­ firmed the fundamental validity of a theoretical version, first proposed via E. N. Parker, predicting a continuing, swift growth of the sunlight corona. the next decade has visible a major development in either the breadth and class of sunlight wind observations; the houses of the interplanetary plasma close to the orbit of the earth are actually recognized in nice element. the idea of the coronal ex­ pansion has additionally been hugely refilled either within the feel of together with extra actual approaches, and of treating extra sensible (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 fast improvement. the final word objective is, after all, the translation of saw sun wind phenomena because the results of simple actual tactics happening within the coronal and interplanetary plasma and because the common manifestations of sun houses and constructions. This strategy implies an emphasis upon the "large-scale" good points published via the observations. It calls for large use of the suggestions and strategies of fluid mechanics.

Show description

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Extra resources for Coronal Expansion and Solar Wind

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26265, where re is the critical radius. This restriction acts as an additional boundary condition and the boundary value problem, as stated above, would be overdetermined. A proper specification of boundary conditions for this class of solution then involves choice of only one of the "coronal conditions" no and To; choice of one effectively determines a single permissible value of the other (as implied in the above description of the relationship among the different classes of solutions). :, and the single independent variable, the dimensionless heliocentric position X = rlre- Specification of the location of the critical radius re then determines the physical variables u, T, and n (through the mass flux integral) at all heliocentric positions.

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).

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.

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