HR: 1330h
AN: SH42B-0530    [PDF]
TI: Magnetic Element Tracking and the Small-Scale Solar Dynamo
AU: * Lamb, D
EM: derek.lamb@colorado.edu
AF: University of Colorado, c/o APS Department, Campus Box 391, Boulder, CO 80309-0391 United States
AU: DeForest, C E
EM: deforest@boulder.swri.edu
AF: Southwest Research Institute, 1050 Walnut Street, Suite 400, Boulder, CO 80302 United States
AB: We have developed flux concentration tracking software to track and identify flux concentration behavior and origin events in photospheric magnetogram sequences. The tracking software is switchable to test and compare the behavior of two existing tracking codes, those of Hagenaar et al. (1999) and Parnell (2002). We present initial results from the use of the software on a deep-field sequence of MDI magnetograms. In particular, the two tracking methods yield significantly different distributions of flux concentration sizes. Furthermore, based on the ratio of coherent and incoherent origin of magnetic flux concentrations in a sequence of deep-field MDI magnetograms, we conclude that ephemeral regions are not typically formed by emergence but rather by random coalescence of groups of smaller, unresolved flux concentrations. Hence, the size distribution of the solar network magnetic field is not determined by the scale of the small-scale dynamo but rather by the clustering statistics of magnetic field elements in the surface flow field.
DE: 7509 Corona
DE: 7524 Magnetic fields
DE: 7529 Photosphere
DE: 7594 Instruments and techniques
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting