DYNAMIC-RESPONSES TO MAGNETIC RECONNECTION IN SOLAR ARCADES

We present a numerical simulation of the interaction between two line dipoles through magnetic reconnection in the lower solar atmosphere, a process believed to be the origin of many manifestations of solar act ivity. This work differs from previous studies in that the held is she ared asymmetrically and that the dipoles have markedly unequal held st rengths. This calculation already yielded one key discovery, denoted r econnection driven current filamentation, as described in a previous A strophysical Journal letter. In this paper we focus on the chromospher ic and coronal dynamics resulting from the shear-driven reconnection o f unequal dipoles, discuss the important implications for chromospheri c eruptions, compare our calculation with high-resolution Normal Incid ence X-Ray Telescope observations of a surge, and contrast our results with the predictions of ''fast reconnection'' models.