SUMMARY
The research sequence on which this thesis is based is typical of work in this field. The design of the experimental apparatus and the data acquisition during the course of the Mariner V mission pre- ceeded the work described here. Beginning with the digitalized magnetometer readings from the spacecraft, a reduction procedure
(including an evaluation of the quality of each observation) was car- ried out to organize the data into a form convenient for detailed analy-
sis. Good quality data were then plotted over a wide range of time scales, and a detailed and· extensive comparison was made between the field data and plasma data generously provided by the plasma experimenters, H. S. Bridge, A. J. Lazarus, and C. W. Snyder.
Using both types of data, the Alfve'n waves were identified, and their frequency of occurrence, direction of propagation, and patterns of occurrence with respect to the large scale stream structures were determined. On the basis of these observations, a qualitative model for the origins of the waves and their relation to the streaming pro- perties of the wind was developed. Although not quantitative, the model serves to organize the large amount of data into a reasonably
simple picture, and provides the basis for more quantitative analysis.
Observationally speaking, the properties of the waves at 1 a. u.
are reasonably well established for this portion of the solar cycle (1967). The areas of significant future interest are long term obser-
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vations at 1 a. u. and observations in regions closer to and further from the sun. It is obviously of importance to measure
oB/B
overas wide a range of solar distances as possible, since the ratio is a measure of both initial wave amplitudes close to the sun and damp- ing and propagation effects of the waves far from the sun. The de- tailed observational behavior of the waves far beyond the orbit of the earth (where the magnetic field becomes tightly wound in the classic spiral) is of particular interest. The proposed Pioneers F and G missions (Jupiter 1972-74) and the Mariner Mercury-Venus mission ( 1973) will thus be invaluable for observational studies of
solar wind wave properties.
From a more theoretical point of view, we have investigated the properties of a simplified wind model which includes wave energy fluxes. Although the model is unrealistic in that it assumes a single fluid plasma with no wave damping, it provides useful insight into the qualitative effects of the observed waves on the actual solar wind.
The next step is a two fluid model with a more sophisticated treat- ment of the energy transport equations (including wave damping). The effects of the rotation of the sun and the spiral field patterns on wave driven solutions is also of considerable interest. The spiraling of the magnetic field should have little effect on the solutions inside
1 a. u., but probably will have a large effect beyond 1 to 2 a. u. A more fundamental problem is the nature of the processes which gen- erate the waves at or near the sun. This question is of obvious inter- est for both solar and interplanetary physics.
In conclusion, the thesis has resolved many observational points and given some consideration to the theoretical points these observations raise. The results provide the basis of and suggest possibilities for future investigations, both observational and theore- tical.
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