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SUMMARY:Numerical modeling of observed solar eruptions - Guillaume Aulanie
 r (Observatoire de Paris-Meudon)
DTSTART:20120528T150000Z
DTEND:20120528T160000Z
UID:TALK37725@talks.cam.ac.uk
CONTACT:Jérôme Guilet
DESCRIPTION: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 1
 0^31-33 ergs of magnetic energy in the solar corona. Part of this goes int
 o the expulsion of a coronal mass ejection (CME) towards the interplanetar
 y medium. Most of the rest is used to accelerate particles\, presumably as
  a result of magnetic reconnecion occurring in the corona. Some of the par
 ticles propagate from the corona down to the solar surface. The chromosphe
 ric impact sites of particles form bright flare ribbons\, from which plasm
 a 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 ex
 plain these features. On the other hand\, EUV spectroscopy with SOHO and H
 INODE has allowed to quantify the plasma evaporation and its strong height
  dependence. Nevertheless\, the full magnetic picture is still lacking : s
 everal triggering mechanisms for CMEs are still debated\; and the 3D prope
 rties of the flare reconnection are just starting to be studied. I will ex
 plain the recent efforts from our group in building a comprehensive and ob
 servationally-driven numerical model for flares and CMEs. Also\, I will sh
 ow results concerning the formation of coronal sigmoids\, the triggering o
 f CMEs\, and the occurrence of a strong-to-weak magnetic shear transition 
 in coronal post-flare loops\, and of electric currents within chromospheri
 c flare ribbons. Finally\, I will discuss possible EUV observations to tes
 t some of the model predictions.
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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