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Chromospheric magnetic fields of an active region filament

Published online by Cambridge University Press:  27 June 2012

M. Faurobert ,
C. Fang ,
T. Corbard ,
Z. Xu ,
S. Solanki  and
A. Lagg
Z. Xu
Affiliation:
Yunnan Astronomical Observatory, CAS, Kunming, 650011 Yunnan, China
S. Solanki
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
A. Lagg
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
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Abstract

Vector magnetic fields of an active region filament are co-spatially and co-temporally mapped in photosphere and upper chromosphere, by using spectro-polarimetric observations made by Tenerife Infrared Polarimeter (TIP II) at the German Vacuum Tower Telescope (VTT). A Zeeman-based ME inversion is performed on the full Stokes vectors of both the photospheric Si I 1082.7 nm and the chromospheric He I 1083.0 nm lines. We found that the strong magnetic fields, with the field strength of 600 − 800 G in the He I line formation height, are not uncommon among AR filaments. But such strong magnetic field is not always found in AR filaments.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 55: 4th French-Chinese Meeting on Solar Physics - Understanding Solar Activity: Advances and Challenges , 2012 , pp. 163 - 168
Copyright
© EAS, EDP Sciences 2012

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