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Solar eruptions are explosive release of coronal magnetic field energy asmanifested in solar flares and coronal mass ejection. Observations have shownthat the core of eruption-productive regions are often a sheared magneticarcade, i.e., a single bipolar configuration, and, particularly, thecorresponding magnetic polarities at the photosphere are elongated along astrong-gradient polarity inversion line (PIL). It remains unclear whatmechanism triggers the eruption in a single bipolar field and why the one witha strong PIL is eruption-productive. Recently, using high accuracy simulations,we have established a fundamental mechanism of solar eruption initiation that abipolar field as driven by quasi-static shearing motion at the photosphere canform an internal current sheet, and then fast magnetic reconnection triggersand drives the eruption. Here we investigate the behavior of the fundamentalmechanism with different photospheric magnetic flux distributions, i.e.,magnetograms, by combining theoretical analysis and numerical simulation. Ourstudy shows that the bipolar fields of different magnetograms, as shearedcontinually, all exhibit similar evolutions from the slow storage to fastrelease of magnetic energy in accordance with the fundamental mechanism, whichdemonstrates the robustness of the mechanism. We further found that themagnetograms with stronger PIL produce larger eruptions, and the key reason isthat the sheared bipolar fields with stronger PIL can achieve morenon-potentiality, and their internal current sheet can form at a lower heightand with a larger current density, by which the reconnection can be moreefficient. This also provides a viable trigger mechanism for the observederuptions in active region with strong PIL.

Numerical Simulation of a Fundamental Mechanism of Solar Eruption with Different Magnetic Flux Distributions