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Filament Shape and Coronal Magnetic Field Structure View all abstracts by submitter

Boris Filippov   Submitted: 2015-10-16 02:30

Solar filament shape in projection on disc depends on the structure of the coronal magnetic field. We calculate the position of polarity inversion lines (PILs) of coronal potential magnetic field at different heights above the photosphere, which compose the magnetic neutral surface, and compare with them the distribution of the filament material in Hα chromospheric images. We found that the most of the filament material is enclosed between two polarity inversion lines (PILs), one at a lower height close to the chromosphere and one at a higher level, which can be considered as a height of the filament spine. Observations of the same filament on the limb by the STEREO spacecraft confirm that the height of the spine is really very close to the value obtained from the PIL and filament border matching. Such matching can be used for filament height estimations in on-disk observations. Filament barbs are housed within protruding sections of the low-level PIL. On the base of simple model, we show that the similarity of the neutral surfaces in potential and non-potential fields with the same sub-photospheric sources is the reason for the found tendency for the filament material to gather near the potential-field neutral surface.

Authors: B. Filippov

Publication Status: Accepted for publication in MNRAS
Last Modified: 2015-10-17 09:57
Go to main E-Print page  Evolution of solar active regions: Detecting the emergence of new magnetic field through multifractal segmentation  SOLAR RADIUS VARIATIONS: AN INQUISITIVE WAVELENGTH DEPENDENCE  Edit Entry  Download Preprint  Delete Entry 

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