Solar Physics

, Volume 286, Issue 1, pp 241–253 | Cite as

Study of a Prominence Eruption using PROBA2/SWAP and STEREO/EUVI Data

  • M. MierlaEmail author
  • D. B. Seaton
  • D. Berghmans
  • I. Chifu
  • A. De Groof
  • B. Inhester
  • L. Rodriguez
  • G. Stenborg
  • A. N. Zhukov


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.


Prominences dynamics Coronal mass ejections, initiation and propagation 



M.M. would like to acknowledge S. Patsourakos for providing the program on spline smoothing and for productive discussions in using this program. She would like to thank also W. Thompson and N. Rich for providing the programs on EUVI pointing correction and height–time measurements. The authors also thank B. Kliem for helpful discussions of our analysis of this event. M.M. thanks MPS for financial support in carrying out this work. Part of her work was also covered from the project TE 73/11.08.2010. We acknowledge the use of PROBA2/SWAP and STEREO/SECCHI data. SWAP is a project of the Centre Spatial de Liège and the Royal Observatory of Belgium funded by the Belgian Federal Science Policy Office (BELSPO). The SECCHI data used here were produced by an International Consortium of the Naval Research Laboratory (USA), Lockheed–Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck Institute for Solar System Research (Germany), Centre Spatiale de Liège (Belgium), Institut d’Optique Theorique et Appliquée (France), Institut d’Astrophysique Spatiale (France).


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Copyright information

© Springer Science+Business Media B.V. 2012

Authors and Affiliations

  • M. Mierla
    • 1
    • 2
    • 3
    Email author
  • D. B. Seaton
    • 2
  • D. Berghmans
    • 2
  • I. Chifu
    • 4
    • 5
  • A. De Groof
    • 6
  • B. Inhester
    • 4
  • L. Rodriguez
    • 2
  • G. Stenborg
    • 7
  • A. N. Zhukov
    • 2
    • 8
  1. 1.Institute of Geodynamics of the Romanian AcademyBucharestRomania
  2. 2.Solar-Terrestrial Center of Excellence – SIDCRoyal Observatory of BelgiumBrusselsBelgium
  3. 3.Research Center for Atomic Physics and Astrophysics, Faculty of PhysicsUniversity of BucharestBucharestRomania
  4. 4.Max-Planck Institute for Solar System ResearchKatlenburg-LindauGermany
  5. 5.Astronomical Institute of the Romanian AcademyBucharestRomania
  6. 6.European Space Agency/Royal Observatory of BelgiumBrusselsBelgium
  7. 7.School of Physics, Astronomy and Computational SciencesGeorge Mason UniversityFairfaxUSA
  8. 8.Skobeltsyn Institute of Nuclear PhysicsMoscow State UniversityMoscowRussia

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