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Titlebook: Basic Mechanisms of Solar Activity; V. Bumba,J. Kleczek Book 1976 International Astronomical Union 1976 Corona.Main sequence.Photosphere.R

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期刊全稱Basic Mechanisms of Solar Activity
影響因子2023V. Bumba,J. Kleczek
視頻videohttp://file.papertrans.cn/182/181067/181067.mp4
學(xué)科分類International Astronomical Union Symposia
圖書封面Titlebook: Basic Mechanisms of Solar Activity;  V. Bumba,J. Kleczek Book 1976 International Astronomical Union 1976 Corona.Main sequence.Photosphere.R
影響因子Our first attempt to organize a Symposium on solar activity was made at the lAO General Assembly in Brighton 1970. There, at the session of Commission 10, we proposed to organize a Symposium which would stress the observational aspects of solar activity. It was our hope that such a Symposium might stimulate studies of those important problems in solar physics which for a long time had been neglected in overall scientific discussion. Although a provisional date for the Symposium was then decided, it did not take place to avoid overlapping with other lAO activities. At the session of Commission 10 in Sydney -on the occasion of the XVth lAO General Assembly in 1973 -we repeated our proposal and forwarded the invitation of the Czechoslovak Academy of Sciences to organize the Symposium in Prague. Both were accepted. During the discussions about the programme of the Symposium -enthusiastically promoted by the late president of Commission 10, Prof. K. O. Kiepenheuer -it was decided to change slightly its subject. The theoreti- cal problems were stressed and the majority of the Scientific Organizing Committee agreed not to deal with short-lived phenomena of the solar activity or with indiv
Pindex Book 1976
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Materialien zu Einem Zerfall der Werte,actly what has been predicted by a numerical solar cycle model driven by the dynamo action of the global convection. Another axisymmetric field is also derived by averaging over longitude the absolute value of the magnetic field after subtracting the poloidal field. This field corresponds to the tor
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Small-Scale Solar Magnetic Fieldsotosphere, and the life-time of the smallest flux elements is very short. The observations further suggest that most of the magnetic flux in quiet regions is supplied directly from below the solar surface rather than being the result of turbulent diffusion of active-region magnetic fields.
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Long Term Evolution of Solar Sector Structurein solar longitude of about 100° and a synodic rotation period of about 28 to 29 days. This 28.5 day structure is usually most prominent during a few years near sunspot maximum. Some preliminary comparisons of these observed solar structures with theoretical considerations are given.
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