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Title:
Study of a Prominence Eruption using PROBA2/SWAP and STEREO/EUVI Data
Authors:
Mierla, M.; Seaton, D. B.; Berghmans, D.; Chifu, I.; De Groof, A.; Inhester, B.; Rodriguez, L.; Stenborg, G.; Zhukov, A. N.
Affiliation:
AA(Institute of Geodynamics of the Romanian Academy; Solar-Terrestrial Center of Excellence - SIDC, Royal Observatory of Belgium), AB(Solar-Terrestrial Center of Excellence - SIDC, Royal Observatory of Belgium), AC(Solar-Terrestrial Center of Excellence - SIDC, Royal Observatory of Belgium), AD(Max-Planck Institute for Solar System Research; Astronomical Institute of the Romanian Academy), AE(European Space Agency/Royal Observatory of Belgium), AF(Max-Planck Institute for Solar System Research), AG(Solar-Terrestrial Center of Excellence - SIDC, Royal Observatory of Belgium), AH(School of Physics, Astronomy and Computational Sciences, George Mason University), AI(Solar-Terrestrial Center of Excellence - SIDC, Royal Observatory of Belgium; Skobeltsyn Institute of Nuclear Physics, Moscow State University)
Publication:
Solar Physics, Volume 286, Issue 1, pp.241-253 (SoPh Homepage)
Publication Date:
08/2013
Origin:
SPRINGER
Keywords:
Prominences dynamics, Coronal mass ejections, initiation and propagation
Abstract Copyright:
(c) 2013: Springer Science+Business Media B.V.
DOI:
10.1007/s11207-012-9965-0
Bibliographic Code:
2013SoPh..286..241M

Abstract

Observations of the early rise and propagation phases of solar eruptive prominences can provide clues about the forces acting on them through the behavior of their acceleration with height. We have analyzed such an event, observed on 13 April 2010 by SWAP on PROBA2 and EUVI on STEREO. A feature at the top of the erupting prominence was identified and tracked in images from the three spacecraft. The triangulation technique was used to derive the true direction of propagation of this feature. The reconstructed points were fitted with two mathematical models: i) a power-law polynomial function and ii) a cubic smoothing spline, in order to derive the accelerations. The first model is characterized by five degrees of freedom while the second one is characterized by ten degrees of freedom. The results show that the acceleration increases smoothly, and it is continuously increasing with height. We conclude that the prominence is not accelerated immediately by local reconnection, but rather is swept away as part of a large-scale relaxation of the coronal magnetic field.
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