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We study the magnetic field structures of hard X-ray sources and flareribbons of the M1.1 flare in active region NOAA 10767 on 2005 May 27. We havefound in a nonlinear force-free field extrapolation, over the same polarityinversion line, a small pre-eruptive magnetic flux rope located next to shearedmagnetic arcades. Ramaty High Energy Solar Spectroscopic Imager (RHESSI) andTransition Region and Coronal Explorer (TRACE) observed this confined flare inthe X-ray bands and ultraviolet (UV) 1600 \AA \ bands, respectively. In thisevent magnetic reconnection occurred at several locations. It first started atthe location of the pre-eruptive flux rope. Then, the observations indicatethat magnetic reconnection occurred between the pre-eruptive magnetic flux ropeand the sheared magnetic arcades more than 10 minutes before the flare peak. Itimplied the formation of the larger flux rope, as observed with TRACE. Next,hard X-ray (HXR) sources appeared at the footpoints of this larger flux rope atthe peak of the flare. The associated high-energy particles may have beenaccelerated below the flux rope, in or around a reconnection region. Still, theclose spatial association between the HXR sources and the flux rope footpointsfavors an acceleration within the flux rope. Finally, a topological analysis ofa large solar region including the active regions NOAA 10766 and 10767 showsthe existence of large-scale Quasi-Separatrix Layers (QSLs) before the eruptionof the flux rope. No enhanced emission was found at these QSLs during theflare, but the UV flare ribbons stopped at the border of the closestlarge-scale QSL.

Evolution of Hard X-ray Sources and Ultraviolet Solar Flare Ribbons for a Confined Eruption of a Magnetic Flux Rope