Astronomy and Astrophysics – Astronomy
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21630203k&link_type=abstract
American Astronomical Society, AAS Meeting #216, #302.03; Bulletin of the American Astronomical Society, Vol. 41, p.847
Astronomy and Astrophysics
Astronomy
Scientific paper
Magnetic fields are the dominant fields that determine the static and dynamic properties of the solar corona. The coronal mass ejections (CMEs) involve the release of the magnetic energy stored in the magnetic field. Therefore, analyzing the magnetic field could help to understand the nature of CMEs. One of the more promising coronal magnetic field measurement methods that have been successfully demonstrated is the spectropolarimetric observations of the Fe XIII 10747 A forbidden emission line (Lin, Penn & Tomczyk 2000; Lin, Kuhn & Coulter 2004; Tomczyk et al. 2007) formed due to Hanle and Zeeman effects. However, these measurements are integrated over line-of-sight (LOS). Therefore it is impossible to determine the configuration of the coronal magnetic field from a single observation (single viewing direction).
Vector tomography based on polarimetric observations of the forbidden coronal emission lines can reconstruct the coronal magnetic field when the observations are obtained from several viewing directions. As the tomography method requires observations from many directions, a rigid rotation of the coronal structures during a half of solar rotation is assumed. However, many pre-CME magnetic configurations evolve more rapidly causing significant reduce in the number of available observing directions. Here we study the sensitivity of the vector tomographic inversion to possible pre-CME coronal magnetic field configurations and the number of available observing directions. We show that the vector tomography techniques has the potential to resolve the 3D coronal non-potential magnetic field structure.
Davila Javier
Inhester Bernd
Kramar Maxim
Lin Hainan
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