HR: 12:05h
AN: SH42A-07    [Abstracts]
TI: 3D Reconstruction of the Electron Density in the Corona from COR1 STEREO Observations
AU: * Kramar, M
EM: kramar@helio.gsfc.nasa.gov
AF: The Catholic University of America, NASA-GSFC, Code 671, Greenbelt, MD 20771, United States
AU: * Kramar, M
EM: kramar@helio.gsfc.nasa.gov
AF: NASA-GSFC, Code 671, Greenbelt, MD 20771, United States
AU: Jones, S
EM: shaelatoo@yahoo.com
AF: NASA-GSFC, Code 671, Greenbelt, MD 20771, United States
AU: Jones, S
EM: shaelatoo@yahoo.com
AF: University of Maryland, Department of Physics, College Park, MD 20742, United States
AU: Davila, J
EM: Joseph.M.Davila@nasa.gov
AF: NASA-GSFC, Code 671, Greenbelt, MD 20771, United States
AU: Inhester, B
EM: inhester@mps.mpg.de
AF: Max-Planck Institut fuer Sonnensystemforschung, Max-Plank-Str. 2, Katlenburg-Lindau, 37191, Germany
AB: We present 3D reconstruction for the electron density in the corona based on the COR1 STEREO observations. The reconstruction is performed by using regularized tomography inversion method.
Since the solar corona is optically thin, coronal observations are essentially integrated over the line-of-sight (LOS). It is therefore impossible to resolve the structure of the corona along the LOS if observations are provided from a single view direction. Observations from different view positions are necessary to reconstruct 3D coronal structure and is the essence of the tomography inversion method. When having observations only from a single view direction, a rigid rotation of the coronal density structures with the Sun about the ecliptic must be assumed in order to apply the tomography technique. As a consequence, only structures which are stationary over half a solar rotation can be reconstructed. The STEREO observations allow us to reduce this stationarity assumption. For reconstruction we choose a period when the Sun is relatively quite. However some active events occurred, and we need to skip the data for these events. Therefore, in order to stabilize the reconstruction, the smoothness factor was used as regularization constraint during the inversion.
DE: 7509 Corona
DE: 7524 Magnetic fields
DE: 7594 Instruments and techniques
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting