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Critical parameters at the onset of solar eruptions


Zuccarello Francesco




Auteur(s) supplémentaire(s)Aulanier Guillaume, Gilchrist Stuart


Magnetic flux ropes are topological structures consisting of twisted magnetic field lines that globally wrap around an axis. 
The torus instability model predicts that a magnetic flux rope of major radius $R$ undergoes an eruption when its axis 
reaches a location where the decay index $-d(\ln B_{ex})/d(\ln R)$ of the ambient magnetic field $B_{ex}$ is larger than a 
critical value. In the current-wire model, the critical value depends on the thickness and time-evolution of the current channel. 
We use magneto-hydrodynamic (MHD) simulations to investigate if the critical value of the decay index at the onset of the eruption 
is affected by the magnetic flux rope's internal current profile and/or by the particular pre-eruptive photospheric dynamics. 
The evolution of an asymmetric, bipolar active region is driven by applying different classes of photospheric motions.
We find that the critical value of the decay index at the onset of the eruption is not significantly affected by either the 
pre-erupitve photospheric evolution of the active region or by the resulting different magnetic flux ropes. 
As in the case of the current-wire model, we find that there is a `critical range' $ [1.3-1.5]$, rather 
than a `critical value' for the onset of the torus instability. This range is in good agreement with the 
predictions of the current-wire model, despite the inclusion of line-tying effects and the occurrence 
of tether-cutting magnetic reconnection.

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