Physics
Scientific paper
Nov 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996nawg.1996..234s&link_type=abstract
Nachr. Akad. Wiss. Göttingen II, Jahrg. 1996, Nr. 4, p. 234 - 240
Physics
Solar Convective Zone: Magnetic Flux Tubes, Solar Convective Zone: Solar Activity Cycles, Solar Convective Zone: Sunspots
Scientific paper
The observed properties of sunspot groups on the surface of the Sun are consistent with the concept of magnetic flux tubes emerging from deep within the solar convection zone. Magnetic flux tubes are generated and storage in mechanical equilibrium in a subadiabatically stratified overshoot layer below the convection zone; they become unstable with respect to an undulatory (Parker-type) instability once the field strength exceeds a critical value; flux loops form, move through the convection zone and give rise to bipolar sunspot regions when they emerge at the surface. Both the stability criteria and the constraints set by the observed properties of sunspot groups (orientation, tilt angle, asymmetry, proper motions) require that the field strength at the bottom of the convection zone should be of the order of 105G, an order of magnitude larger than the equipartition field strength with respect to the convective flows. This result has profound consequences for dynamo models for the solar cycle.
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