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Patterns of active region magnetic field development

Published online by Cambridge University Press:  14 August 2015

V. Bumba ,
R. Howard ,
M.J. Martres  and
I. Soru-Iscovici
V. Bumba
Affiliation:
Astronomical Institute, Ondřejov, Czechoslovakia
R. Howard
Affiliation:
Astronomical Institute, Ondřejov, Czechoslovakia
M.J. Martres
Affiliation:
Observatoire de Paris-Meudon, (92) Meudon, France
I. Soru-Iscovici
Affiliation:
Observatoire de Paris-Meudon, (92) Meudon, France

Abstract

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We discuss some characteristics of the appearance and development of magnetic fields within active regions as well as the large-scale ordering of activity into complexes of activity. It is not possible to separate a study of the evolution of active regions from a study of the model of the activity cycle. Many of the results obtained in the last few years concerning the development of active regions and large-scale activity have not been easily explained within any of the solar activity models. A chronological scheme of the development of a ‘typical’ C- or D-type active region is presented. We point out that the appearance of magnetic flux at the solar surface seems always to be a relatively rapid event, occurring during the course of a day or so. If the region does not receive more magnetic flux to make it a large region or if there is not a resurgence of activity later in its lifetime, the rest of the development is a gradual expansion and mixing of magnetic flux with the surrounding background field pattern.

Type
Part I: General Development of an Active Region
Information
Symposium - International Astronomical Union , Volume 35: Structure and Development of Solar Active Regions , 1968 , pp. 11 - 24
Copyright
Copyright © Reidel 1968 

References

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