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Formation and evolution of an active region filament

Published online by Cambridge University Press:  06 January 2014

Christoph Kuckein ,
Rebeca Centeno  and
Valentín Martínez Pillet
Christoph Kuckein
Affiliation:
Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482, Potsdam, Germany. email: ckuckein@aip.de Instituto de Astrofísica de Canarias (IAC), Vía Láctea s/n, 38205, La Laguna, Tenerife, Spain
Rebeca Centeno
Affiliation:
High Altitude Observatory (NCAR), Boulder, CO 80301, USA
Valentín Martínez Pillet
Affiliation:
National Solar Observatory (NSO), Sunspot, NM 88349, USA
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Abstract

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Several scenarios explaining how filaments are formed can be found in literature. In this paper, we analyzed the observations of an active region filament and critically evaluated the observed properties in the context of current filament formation models. This study is based on multi-height spectropolarimetric observations. The inferred vector magnetic field has been extrapolated starting either from the photosphere or from the chromosphere. The line-of-sight motions of the filament, which was located near disk center, have been analyzed inferring the Doppler velocities. We conclude that a part of the magnetic structure emerged from below the photosphere.

Keywords

Sun: filamentsprominencesSun: photosphereSun: chromosphereSun: magnetic fieldstechniques: polarimetric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S300: Nature of Prominences and their role in Space Weather , June 2013 , pp. 40 - 43
Copyright
Copyright © International Astronomical Union 2013 

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