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Numerical modeling of observed solar eruptions

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If you have a question about this talk, please contact Jérôme Guilet.

Solar eruptions are the most energetic phenomena of the solar system. In time-scales of the order of 1 minute to 1 hour, they release 10^31-33 ergs of magnetic energy in the solar corona. Part of this goes into the expulsion of a coronal mass ejection (CME) towards the interplanetary medium. Most of the rest is used to accelerate particles, presumably as a result of magnetic reconnecion occurring in the corona. Some of the particles propagate from the corona down to the solar surface. The chromospheric impact sites of particles form bright flare ribbons, from which plasma evaporation gradually fills post-flare coronal loops with hot material. Strong EUV and SXR emissions are observed in these flare ribbons and loops. On the one hand, a 2D standard model has long since been proposed to explain these features. On the other hand, EUV spectroscopy with SOHO and HINODE has allowed to quantify the plasma evaporation and its strong height dependence. Nevertheless, the full magnetic picture is still lacking : several triggering mechanisms for CMEs are still debated; and the 3D properties of the flare reconnection are just starting to be studied. I will explain the recent efforts from our group in building a comprehensive and observationally-driven numerical model for flares and CMEs. Also, I will show results concerning the formation of coronal sigmoids, the triggering of CMEs, and the occurrence of a strong-to-weak magnetic shear transition in coronal post-flare loops, and of electric currents within chromospheric flare ribbons. Finally, I will discuss possible EUV observations to test some of the model predictions.

This talk is part of the DAMTP Astrophysics Seminars series.

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