Testing the vector tomography method for 3D reconstruction of the coronal magnetic field for different coronal field models

Details Testing the vector tomography method for 3D reconstruction of the coronal magnetic field for different coronal field models Testing the vector tomography method for 3D reconstruction of the coronal magnetic field for different coronal field models

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.

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