Physics
Scientific paper
Oct 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.505..113v&link_type=abstract
In: SOLMAG 2002. Proceedings of the Magnetic Coupling of the Solar Atmosphere Euroconference and IAU Colloquium 188, 11 - 15 Jun
Physics
12
Solar Magnetic Fields, Magnetic Flux Emergence, Magnetic Diffusion, Magnetic Cancellation
Scientific paper
This review is focused on observations and theoretical advances on large-scale flux emergence and decay, which forms and dominates the magnetic field patterns on the Sun. The basic characteristics of emerging flux (asymmetry, inclination to the vertical, twist, sea-serpent-like appearance in the early stage of flux emergence in the photosphere) are described together with the results of relevant MHD simulations, which help us to interpret these observations. Magnetic flux emergence is far from being a random process in the active belt: it has a grouping (nesting) tendency, which has important implications for the operation of the solar dynamo. As soon as active regions are fully formed, they start decaying. Their magnetic flux gradually speads over an ever-increasing area and gets removed from the photosphere via small scale processes (e.g. Ohmic dissipation and flux cancellation, including flux submergence). Emergence of U-loops may play an important role in the removal of large-scale flux from the photopshere.
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