Thinkshop12

MHD Simulation of a Confined Solar Filament Eruption

Alshaimaa Hassanin (Potsdam university – Institut für Physik und Astronomie)

Abstract. Toeroek & Kliem’s non- resistive MHD simulation (2005) showed , by using the magnetic flux rope equilibrium by Titov & Demoulin (1999) as the initial condition, a good agreement with event May 2002 . Drawing upon Toeroek et al. Model, we explore more the external toroidal and poloidal field with less average twisting flux rope and in addition we go after the rest of the simulation at which Toereok et al . stopped 2005 . This is characterized by a sequence of reconnection events involving the magnetic flux of the rope (the filament) as well as the ambient, overlying flux. First, the top part of the rope reconnects with the ambient flux. Second, the two legs of the split rope approach each other and reconnect. This leads to the reformation of a flux rope, with less twist, and also restores the overlying flux. Further minor reconnection occurs under the new rope, completing its reformation. We find that the shapes of the field lines that reconnect in steps 1 and 2 correspond well to the observed flare loops. The flare loops show considerable brightness, although the eruption remained confined. This appears plausible from the fact that these loops were involved in two phases of reconnection, each of which contributed to the heating of the flare plasma. The reformation of the flux rope may yield a path to homologous flare events. Overall, the sequence of ideal MHD instability and magnetic reconnection corresponds well to the observations of the eruption.

Poster