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Magnetic reconnection driven by filament eruption in the 7 June 2011 event

  • L. van Driel-Gesztelyi (a1) (a2) (a3), D. Baker (a1), T. Török (a4), E. Pariat (a2), L. M. Green (a1), D. R. Williams (a1), J. Carlyle (a1), G. Valori (a2), P. Démoulin (a2), S. A. Matthews (a1), B. Kliem (a5) and J.-M. Malherbe (a2)...

Abstract

During an unusually massive filament eruption on 7 June 2011, SDO/AIA imaged for the first time significant EUV emission around a magnetic reconnection region in the solar corona. The reconnection occurred between magnetic fields of the laterally expanding CME and a neighbouring active region. A pre-existing quasi-separatrix layer was activated in the process. This scenario is supported by data-constrained numerical simulations of the eruption. Observations show that dense cool filament plasma was re-directed and heated in situ, producing coronal-temperature emission around the reconnection region. These results provide the first direct observational evidence, supported by MHD simulations and magnetic modelling, that a large-scale re-configuration of the coronal magnetic field takes place during solar eruptions via the process of magnetic reconnection.

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References

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Lemen, J. R., Title, A. M., Akin, D. J., et al., 2012, Solar Phys. 275, 17
van Driel-Gesztelyi, L., Baker, D., Török, T., Pariat, E., Green, L. M., Williams, D. R., Carlyle, J., Valori, G., Démoulin, P., Matthews, S. A., Kliem, B., & Malherbe, J.-M. 2013, ApJ, submitted.
Williams, D. R., Baker, D., & van Driel-Gesztelyi, L. 2013, ApJ, 764, 165
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Magnetic reconnection driven by filament eruption in the 7 June 2011 event

  • L. van Driel-Gesztelyi (a1) (a2) (a3), D. Baker (a1), T. Török (a4), E. Pariat (a2), L. M. Green (a1), D. R. Williams (a1), J. Carlyle (a1), G. Valori (a2), P. Démoulin (a2), S. A. Matthews (a1), B. Kliem (a5) and J.-M. Malherbe (a2)...

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