Other
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.2404f&link_type=abstract
American Astronomical Society Meeting 210, #24.04; Bulletin of the American Astronomical Society, Vol. 39, p.129
Other
Scientific paper
We present a set of 3D spherical shell anelastic MHD simulations of the buoyant rise of magnetic flux tubes through the solar convective envelope (up to a depth of 20Mm below the photosphere). It is found that a twisted flux tube when arched upward due to buoyancy will develop a writhe of the tube axis and thus produce a tilt at the apex. This twist induced tilt is counter-clockwise (clock-wise) when viewed from the top for a flux tube with a left-handed (right-handed) twist. On the other hand, the Coriolis force acting on the diverging, expanding motion at the apex of a rising flux tube will drive a clock-wise (counter-clock-wise) tilt at the tube apex in the northern (southern) hemisphere. Our present 3D MHD simulations show that for tubes with a twist rate that is necessary for a cohesive rise, the twist induced tilt dominates that caused by the Coriolis force, and furthermore, the twist induced tilt is of the wrong direction (opposite to the observed Joy's law) if the twist is left-handed (right-handed) in the northern (southern) hemisphere following the observed hemispheric preference of the sign of active region twist. It is found that in order for the emerging flux tube to show the correct tilt direction (consistent with observations), the initial twist rate of the flux tube needs to be less than a half of that needed for a cohesive rise. We also found that a field strength asymmetry develops with the field in the leading leg (leading in the direction of rotation) of the Omega-shaped emerging tube being stronger than the following, resulting in a more compact flux distribution and a higher peak field strength in the leading polarity of the emerging active region.
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