Abstract We describe the current status of our observational and theoretical comprehension of the fundamental activity mechanism of the sun, whereby subsurface motions slowly drive the coronal magnetic field into a stressed state that may suffer a loss of equilibrium or become disruptively unstable, leading to the rapid release of energy. Our empirical knowledge proceeds from modern measurements of surface magnetic and flow fields. The former, derived from vector magnetograms, can be used to construct a quantitative model (within resolution and accuracy limits) of the coronal field of an active region. The stored magnetic energy and current density can also be computed at this instant in time. The photospheric flow fields can then, in principle, be used to drive the active-region magnetic field to a subsequent higher-energy state. One can then create model three-dimensional computational simulations of these evolutionary motions which show transitions to instability and eruption that are characteristic of observed solar flare activity.
The generation of solar magnetic activity: Photospheric flows and coronal fields
Advances in Space Research ; 13 , 9 ; 15-22
01.01.1993
8 pages
Aufsatz (Zeitschrift)
Elektronische Ressource
Englisch
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