HR: 0830h
AN: SH51C-10    [Abstracts]
TI: Boundary Flows in Solar Active Regions
AU: * Georgoulis, M K
EM: manolis.georgoulis@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AU: LaBonte, B J
EM: barry.labonte@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AB: We present a general technique to calculate the flow field at the altitude where vector magnetic field measurements of solar active regions have been obtained. The velocity field vector is reconstructed fully by solving the ideal induction equation of magnetohydrodynamics for the cross-field velocity component and by utilizing the Doppler velocity information to calculate the field-aligned velocity component. Because solving the induction equation is an under-determined problem, we have formulated our technique in such a way as to provide a unique solution of the induction equation when the vertical (normal to the boundary) component of the cross-field velocity is prescribed. We provide examples of various possible choices for the cross-field vertical velocity and we discuss the respective results. Moreover, we showcase the validity of our technique by predicting the particular area of NOAA active region 8210 from which a flare and a CME were triggered, using the reconstructed velocity field vector.
DE: 7513 Coronal mass ejections
DE: 7519 Flares
DE: 7524 Magnetic fields
DE: 7529 Photosphere
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly