Physics
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.506..781t&link_type=abstract
In: Solar variability: from core to outer frontiers. The 10th European Solar Physics Meeting, 9 - 14 September 2002, Prague, Cze
Physics
1
Mhd, Sun: Activity, Sun: Corona, Sun: Coronal Mass Ejections (Cmes), Sun: Flares, Sun: Magnetic Fields
Scientific paper
We simulate the twisting of initially potential coronal magnetic flux by slow photospheric vortex motions using the compressional, zero-beta ideal MHD equations. The twisted flux tube starts to evolve quasi-statically along a sequence of force-free equilibria, rising slowly and possessing helical shape. As a critical amount of twist is reached, the evolution becomes dynamic and the tube rises and expands rapidly. No neighbouring equilibrium can be found in the simulation domain at this stage of the evolution, as confirmed by relaxation runs. Hence, above the critical twist either the flux tube becomes unstable or neighbouring equilibria rise by enormous amounts for only small additional twist. Both cases would be observed as an eruption. The critical end-to-end twist of the flux tube is found to lie in the range 2.5π < Φc < 3.0π.
Kliem Bernhard
Torok Tibor
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