HR: 0800h
AN: SH32A-0770    [Abstracts]
TI: 3D Magnetic Modeling of Active Regions Using STEREO/EUVI
AU: * Sandman, A
EM: asandman@rice.edu
AF: Rice University, 6100 Main Street, Houston, TX 77005, United States
AU: Aschwanden, M J
EM: aschwand@lmsal.com
AF: Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Palo Alto, CA 94304, United States
AU: Alexander, D
EM: dalex@rice.edu
AF: Rice University, 6100 Main Street, Houston, TX 77005, United States
AU: Wuelser, J
EM: wuelser@lmsal.com
AF: Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Palo Alto, CA 94304, United States
AB: With the recent availability of stereoscopic data from the Extreme Ultraviolet Imager (EUVI) on the Solar Terrestrial Relations Observatory (STEREO) we have an unprecedented opportunity to investigate the accuracy of 3D magnetic field models. These data will be put to best use by modeling techniques that make no assumptions about the nature of the field (that it is potential, force-free, etc.). The Gary-Alexander radial stretching method use a series of transformations to map a simple potential field to a more complicated target field, and compare the transformed field lines with observed coronal structures in the EUV. Unlike many other simulation techniques, this approach requires only that the field remain divergence-free and continuous at the photosphere. Here we apply this transformation method to STEREO/EUVI data. We obtain a 3D potential field extrapolation using an MDI magnetogram, and utilize stereoscopy to derive the 3D field line coordinates from pairs of EUV images at 171Å. By comparing the 3D coordinates of the transformed model field lines with those of the real field lines as seen by EUVI, we can place constraints on the distribution of magnetic field and current in an active region.
DE: 7509 Corona
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting