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The underlying origin of solar eruptive events (SEEs), ranging from giantcoronal mass ejections to small coronal-hole jets, is that the lowest-lyingmagnetic flux in the Sun's corona undergoes the continual buildup of stress andfree energy. This magnetic stress has long been observed as the phenomenon of"filament channels:" strongly sheared magnetic field localized aroundphotospheric polarity inversion lines. However, the mechanism for the stressbuildup - the formation of filament channels - is still debated. We presentmagnetohydrodynamic simulations of a coronal volume that is driven bytransient, cellular boundary flows designed to model the processes by which thephotosphere drives the corona. The key feature of our simulations is that theyaccurately preserve magnetic helicity, the topological quantity that isconserved even in the presence of ubiquitous magnetic reconnection. Althoughsmall-scale random stress is injected everywhere at the photosphere, drivingstochastic reconnection throughout the corona, the net result of the magneticevolution is a coherent shearing of the lowest-lying field lines. This highlycounter-intuitive result - magnetic stress builds up locally rather thanspreading out to attain a minimum energy state - explains the formation offilament channels and is the fundamental mechanism underlying SEEs.Furthermore, this mechanism may be relevant to other astrophysical orlaboratory plasmas.

The Mechanism for the Energy Buildup Driving Solar Eruptive Events