Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980lastr..94..431r&link_type=abstract
L'Astronomie, vol. 94, Oct. 1980, p. 431-437. In French.
Astronomy and Astrophysics
Astronomy
Solar Activity, Solar Magnetic Field, Solar Oscillations, Stellar Mass, Velocity Distribution, Chromosphere, Convection, Photosphere, Solar Atmosphere, Solar Rotation, Sunspots
Scientific paper
The formation and evolution of solar active regions are discussed with emphasis on the role of interactions between the solar magnetic field and mass motions. The generation and persistence of solar magnetic fields due to movements of matter within the sun, and the continual oscillation between poloidal and toroidal global field configurations brought about by differential solar rotation and large scale convection are considered as the source of the solar activity cycle. The transport of magnetic flux tubes to the surface to form active regions is explained in terms of a magnetic Archimedes force. The evolution of active regions is then analyzed, with consideration given to the conditions under which the magnetic fields are neutralized and under which frozen-in magnetic fields develop into sunspots and active regions with large mass motions in the photosphere and chromosphere.
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