Physics – Plasma Physics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh31a1789k&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH31A-1789
Physics
Plasma Physics
[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7833] Space Plasma Physics / Mathematical And Numerical Techniques
Scientific paper
Magnetic fields in the solar corona dominates the gas pressure and therefore determine the static and dynamic properties of the corona. Direct measurement of the coronal magnetic field is one of the most challenging problems in observational solar astronomy and recently had significant progress (Lin et al. 2004; Tomczyk et al. 2008). The polarization of infrared Fe XIII 10747 A forbidden line depends on magnetic field through the Hanle and Zeeman effects. However, because the coronal measurements are integrated over line-of-site (LOS), it is impossible to derive the configuration of the coronal magnetic field from a single observation (from a single viewing direction). The vector tomography techniques based on measurements from several viewing directions has the potential to resolve the 3D coronal magnetic field structure over LOS. Previously, the potential of the method was demonstrated for two basic model field configurations (Kramar et al. 2006). Because of the non-linear character of the Hanle effect, the reconstruction result based on such data is not straightforward and depends on the particular coronal field configuration. Therefore we study here what is the sensitivity of the vector tomographic inversion to more sophisticated (MHD) coronal magnetic field models.
Inhester Bernd
Kramar Maxim
Lin Hainan
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