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A standard model for eruptive flares aims at describing observational 3Dfeatures of the reconnecting coronal magnetic field. Extensions to the 2D modelrequire the physical understanding of 3D reconnection processes at the originof the magnetic configuration evolution. However, the properties of 3Dreconnection without null point and separatrices still need to be analyzed. Wefocus on magnetic reconnection associated with the growth and evolution of aflux rope and associated flare loops during an eruptive flare. We aim atunderstanding the intrinsic characteristics of 3D reconnection in the presenceof quasi-separatrix layers (QSLs), how QSL properties are related to theslip-running reconnection mode in general, and how this applies to eruptiveflares in particular. We studied the slip-running reconnection of field linesin a magnetohydrodynamic simulation of an eruptive flare associated with atorus-unstable flux rope. Field lines associated with the flux rope and theflare loops undergo a continuous series of magnetic reconnection, which resultsin their super-Alfvenic slipping motion. The time profile of their slippagespeed and the space distribution of the mapping norm are shown to be stronglycorrelated. We find that the motion speed is proportional to the mapping norm.Moreover, this slip-running motion becomes faster as the flux rope expands,since the 3D current layer evolves toward a current sheet, and QSLs toseparatrices. The present analysis extends our understanding of the 3Dslip-running reconnection regime. We identified a controlling parameter of theapparent velocity of field lines while they slip-reconnect, enabling theinterpretation of the evolution of post flare loops. This work completes thestandard model for flares and eruptions by giving its 3D properties.

The standard flare model in three dimensions III. Slip-running reconnection properties