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3D Kinematic Evolution of Erupting Filaments

Published online by Cambridge University Press:  27 June 2012

M. Faurobert ,
C. Fang ,
T. Corbard ,
T. Li ,
J. Zhang ,
Y. Zhang  and
S. Yang
T. Li
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
J. Zhang
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
Y. Zhang
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
S. Yang
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
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Abstract

We reconstruct the three-dimensional geometry of erupting filaments using observations from different viewpoints. True kinematic evolution of different locations along the main bodies of filaments is investigated. For the erupting filament on 2009 September 26, the highest point is the fastest in the first half hour, and then the points at the low-latitude leg of the filament become the fastest. However, for the event on 2010 August 1, the highest location always has the largest velocity and acceleration during the eruption process. The propagation of EUV enhancements at the endpoints of the erupting filament is observed clearly, which is attributed to the successive down-flows along the different groups of thread-like structures of the filament. Both the two filaments show non-radial eruptions and move towards low-latitude region. Their latitudinal variation is greater than the longitudinal.

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. 179 - 184
Copyright
© EAS, EDP Sciences 2012

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