Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh44a..01d&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SH44A-01
Physics
7524 Magnetic Fields, 7529 Photosphere, 7536 Solar Activity Cycle (2162)
Scientific paper
Large-scale magnetic field patterns visible at high latitudes on the solar photosphere are thought to form primarily from the poleward transport of flux that has emerged at lower latitudes. It is only a small percentage of this lower-latitude (i.e., active region) flux, however, that makes it to the poles, as much active-region flux cancels during its emergence and subsequent dispersal. This dispersal is characterized by the shearing and advection caused by the surface differential rotation and meridional flows, as well as by constant buffeting by near-surface convection and interactions with nearby flux concentrations. Consequently, these processes can play an important role in the transport of flux to the poles and the buildup of the polar caps, and their nonlinear nature implies that interactions between patterns with differing spatial (and temporal) scales can affect the timing of the formation of the polar cap as well as its overall amplitude. Such possibilities are investigated using a surface flux-transport model, and implications regarding the heliosphere are discussed.
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