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We examine the response of various physical environments representing the solar atmosphere to a magnetic reconnection event. The reconnection is driven by a localized increase of the magnetic diusivity in the current concentration formed between two magnetic fluxes of opposite polarity. The time dependent evolution is then followed by numerically solving the 2-dimensional (2D) dissipative magnetohydrodynamic (MHD) equations, including also eects of thermal conduction, radiative losses, and volumetric heating. This work continues a previous related study (Roussev et al. 2001a), and compares results obtained from exploring dierent initial states. The choice of the initial states is found to be crucial to the dynamics of the reconnection jets. The numerical experiments are aimed at modelling transient events on the quiet Sun, with an emphasis on explosive events. The 2D reconnection experiments presented in this paper are the basis for a detailed analysis on the line synthesis in transition region resonant lines, presented by Roussev et al. (2001b).

Modelling of explosive events in the solar transition region in a 2D environment