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Although accurate at the time of publication, it is no longer being updated. The page may contain broken links or outdated information, and parts may not function in current web browsers.
Owing to the differential rotation of outer solar layers, magnetic field lines within the convection zone in the Sun experience shear, stress, and a resulting magnetic bouyancy. When they break through the visible photospheric surface they float high into the corona, often forming arcades of beautiful arches.
Above is background material for archival reference only.
