By Jacques M. Beckers (auth.), Robert Howard (eds.)
This symposium used to be held on the collage de France in Paris from August 31 to Sep tember four, 1970. The Organizing Committee consisted of V. Bumba, R. Howard (Chairman), ok. O. Kiepenheuer, R. Michard, E. N. Parker, A. B. Severny, V. E. Stepanov, and T. Takakura. The neighborhood Organizing Committee consisted of pass over G. Drouin (Secretary), R. Michard (Chairman), J. -C. Pecker, and J. Rayrole. we're indebted to the school de France for his or her sort hospitality. I desire to exhibit my gratitude to individuals of the Organizing Committee for recommendation and suggestions and to R. Michard and the neighborhood Organizing Committee, who have been accountable for the sleek working of the classes, the distribution and choice of the dialogue sheets, and for a pleasant Wednesday afternoon expedition to Meudon. it's a excitement to thank J. W. Evans, V. E. Stepanov, ok. O. Kiepenheuer, R. G. Giovanelli, T. G. Cowling, V. Bumba, W. C. Livingston, and J. M. Wilcox who kindly served as consultation chairmen. I additionally desire to thank leave out Judy Harstine and John M. Adkins of the Hale Observatories, for precious tips in modifying the lawsuits. This Symposium has been supported financially by way of the foreign Astronomical Union.
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Extra resources for Solar Magnetic Fields
The negative, displaced one frame with respect to the positive, is imaged on to the positive/unexposed film combination and an exposure taken, thus providing a magneto gram. Once the original alignment between the image of the negative and the positive has been established, the remainder of the process is automatic since the separation between each pair of frames to be subtracted is fixed by the beam splitter. Since a subtraction of the correct sense is obtained on only every second frame, every alternate frame must be removed in a subsequent stage of editing.
The following is the result of numerical computation made by Rayrole and myself. Our first question was whether an observed profile in absence of magnetic field may allow to determine the model to be used and its parameters. We found that numerically speaking the S - Sand M - E models are equivalent. That is we found that for each of the three parameters of one model we can find a choice of three parameters for the other model to obtain practically the same profile. Then we introduced the magnetic field but we find again that the two models give similar profiles when using for each model the parameters adjusted as above for the zero field profile.
V 4. The Analysis in the Case of Linear Polarization The interpretation of linear polarization in terms of magnetic fields cannot be made independent of the parameters of line formation. A dependence on the broadening MEASUREMENTS OF MAGNETIC FIELDS 41 mechanism is expected. However for many lines the broadening mechanisms are likely to be identical. Therefore it would be interesting to develop a method where the calibration of polarimetric measurements depends only on the broadening parameters.