Development of solar active regionsThe birth, growth, and decay of solar active regions are described. The appearance of active regions in different atmospheric layers is examined, and the coronal extension of active regions is considered. The use of Skylab soft X-ray and extreme UV observations for studying the complex loop structure of active regions in the solar corona and the sensitive reactions of the upper atmospheric layers to newly emerging flux is explained. It was found that well developed active regions are much bigger in the corona than in the underlying sunspot groups and plages, and that many of the active regions are connected with others through systems of magnetic field lines, occasionally visible in soft X-rays. These interconnections, which may survive several solar rotations, indicate bigger complexes on the sun than one individual active region.
Document ID
19770061356
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Svestka, Z. (American Science and Engineering, Inc. Cambridge, Mass., United States)
Date Acquired
August 9, 2013
Publication Date
January 1, 1976
Subject Category
Solar Physics
Meeting Information
Meeting: International Symposium on Solar-Terrestrial Physics