Authors: Marcel F. Corchado Albelo (University of Colorado Boulder/LASP/NSO), Maria D. Kazachenko (Univeristy of Colorado Boulder/LASP/NSO), Joel T. Dahlin (Univeristy of Maryland/GSFC), Ryan J. French (LASP)

Our understanding of two-ribbon solar flares suggests that three-dimensional (3D) magnetic reconnection, that is with a spatially varying non-reconnecting component (guide field) determines most of the spatial distribution of intense heating sites in the lower solar atmosphere (flare ribbons). Moreover, recent resistive magnetohydrodynamic (RMHD) numerical experiments of magnetic eruption suggest that the structures within a fragmented reconnection site can generate small scale morphological deformations to the flare ribbons (fine structures).  We study the detailed evolution of one of these structures, a plasmoid formed by the resistive oblique tearing mode, due to reconnection and coronal dynamics in a RMHD simulation of a two-ribbon flare. Furthermore, we evaluate how the evolution of the plasmoid affects the development of fine structure, and changes in the net reconnection flux rate.