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We report on observations of conversion of bright filament strands into flareloops during 2012 August 31 filament eruption. Prior to the eruption,individual bright strands composing one of the legs of the filament wereobserved in the 171 A filter channel data of the Atmospheric Imaging Assembly.After the onset of the eruption, one of the hooked ribbons started to propagateand contract, sweeping footpoints of the bright filament strands as well ascoronal loops located close by. Later on, hot flare loops appeared in regionsswept by the hook, where the filament strands were rooted. Timing andlocalization of these phenomena suggest that they are caused by reconnection offield lines composing the filament at the hook, which, to our knowledge, hasnot been observed before. This process is not included in the standard flaremodel (CSHKP), as it does not address footpoints of erupting flux ropes andribbon hooks. It has, however, been predicted using the recentthree-dimensional extensions to the standard flare model. There, the eruptingflux rope can reconnect with surrounding coronal arcades as the hookedextensions of current ribbons sweep its footpoints. This process results information of flare loops rooted in previous footpoints of the flux rope. Ourobservations of sweeping of filament footpoints are well described by thisscenario. In all observed cases, all of the footpoints of the erupting filamentbecame footpoints of flare loops. This process was observed to last for about150 minutes, throughout the whole eruption.

Manifestations of three dimensional magnetic reconnection in an eruption of a quiescent filament: \\ Filament strands turning to flare loops