Abstract
Using a two-dimensional, three-component magnetohydrodynamic model, a numerical study is presented on the disturbance of prominence caused by photospheric magnetic cancellation. Photospheric magnetic cancellation below the prominence transports magnetic flux into the prominence, resulting in an increase of both magnetic flux and helicity in the prominence. The state of the prominence is related to its accumulated magnetic flux (or magnetic helicity). As shown in the numerical results, when δ F (the relative increment of magnetic flux in the prominence) or δ H (the corresponding relative increment of magnetic helicity) is small, the prominence rises and expands only slightly, and remains in contact with the photosphere. On the other hand, when δ F or δ H is large, the prominence is detached from the photosphere and eventually is suspended in the lower corona, leading to the formation of a vertical current sheet below the prominence.
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