Download PDF by E. N. Parker (auth.), V. Bumba, J. Kleczek (eds.): Basic Mechanisms of Solar Activity

By E. N. Parker (auth.), V. Bumba, J. Kleczek (eds.)

ISBN-10: 9027706816

ISBN-13: 9789027706812

ISBN-10: 9401014817

ISBN-13: 9789401014816

Our first try to arrange a Symposium on sun job was once made on the lAO common meeting in Brighton 1970. There, on the consultation of fee 10, we proposed to arrange a Symposium which might rigidity the observational points of sun job. It was once our wish that the sort of Symposium may possibly stimulate stories of these vital difficulties in sun physics which for a very long time were overlooked in total medical dialogue. even if a provisional date for the Symposium was once then determined, it didn't happen to prevent overlapping with different lAO actions. on the consultation of fee 10 in Sydney -on the party of the XVth lAO normal meeting in 1973 -we repeated our inspiration and forwarded the invitation of the Czechoslovak Academy of Sciences to prepare the Symposium in Prague. either have been accredited. through the discussions in regards to the programme of the Symposium -enthusiastically promoted via the overdue president of fee 10, Prof. okay. O. Kiepenheuer -it was once determined to alter a bit of its topic. The theoreti­ cal difficulties have been under pressure and nearly all of the clinical Organizing Committee agreed to not take care of short-lived phenomena of the sun task or with person lively areas. Symposium No. seventy one was once held in Prague from August 25 to August 29, 1975. Its Organizing Committee consisted of V. Bumba (Chairman), W. Deinzer, R. G. Giovanelli, R. Howard, okay. O. Kiepenheuer, M. Kopecky, T. Krause, M. Kuperus, G.

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These rms deviations do not present the accuracy of measurements which is much better, but reflect mainly the random walk of the Ca +-mottles superposed on the drift, due to rotation. Clearly, a straight line representation of the data, resulting in a longitude independent rotation rate, is rather unsatisfactory. A much better fit is obtained by a sinoidal-curve leading to two sectors with faster than average rotation and two sectors with slower than average rotation for each hemisphere. 105kms- 1• There is a 90° phase difference between the sectors of the northern and southern hemisphere.

At the moment a nonsolar cause for the velocity variations cannot be ruled out. Some tests have been made in an attempt to isolate an instrumental origin for the variations, but no means of reproducing the magnitude of the effect has been found. Altering the balance on the photomultiplier tubes at the exit slits so as to offset the line profile can change the derived rotation velocity, but to achieve the magnitude of the observed effect requires an unreasonably large offset - so large that at the extrema it is difficult to hold the line with the line-centering servo.

1972, Solar Phys. 26, 354. Chapman, R. D. and Neupert, W. : 1974, J. Geophys. Res. 79, 4138. : 1970, Solar Phys. 12, 23. Newton, H. W. and Nunn, M. : 1951, Monthly Notices Roy. Astron. Soc. HI, 413. : 1972, J. Geophys. Res. 77, 4027. : 1971, Solar Phys. 18, 72. Wagner, W. : 1975, Astrophys. J. Letters 198, L141. Wilcox, J. M. and Howard, R: 1970, Solar Phys: 13, 251. DISCUSSION Stix: Which latitude of the coronal hole exactly corresponds to the rotation of the interplanetary sector structure?

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Basic Mechanisms of Solar Activity by E. N. Parker (auth.), V. Bumba, J. Kleczek (eds.)

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