Wuppertal 2015 – wissenschaftliches Programm

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EP: Fachverband Extraterrestrische Physik

EP 5: SDO/Sunrise/STEREO

EP 5.6: Vortrag

Dienstag, 10. März 2015, 18:45–19:00, G.10.02 (HS 9)

MHD Simulation of a Confined Solar Filament Eruption — •Alshaimaa Hassanin and Bernhard Kliem — Universität Potsdam- Intsitut für Physik und Astronomie

We present MHD simulations of a confined filament eruption, which produced a solar flare but no coronal mass ejection. The onset of this event (on 2002 May 27) was modeled in Toeroek & Kliem (2005), using the magnetic flux rope equilibrium by Titov & Demoulin (1999) as the initial condition. They found the event to be a good candidate for the occurrence of the helical kink instability. Now we follow the eruption into the main flare phase. 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.