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A filament disappearance event was observed on 22 May 2008 during our recentcampaign JOP 178. The filament, situated in the southern hemisphere, showedsinistral chirality consistent with the hemispheric rule. The event was wellobserved by several observatories in particular by THEMIS. One day before thedisappearance, H$\alpha$ observations showed up and down flows in adjacentlocations along the filament, which suggest plasma motions along twisted fluxrope. THEMIS and GONG observations show shearing photospheric motions leadingto magnetic flux canceling around barbs. STEREO A, B spacecraft with separationangle 52.4 degrees, showed quite different views of this untwisting flux ropein He II 304 \AA\ images. Here, we reconstruct the 3D geometry of the filamentduring its eruption phase using STEREO EUV He II 304 \AA\ images and find thatthe filament was highly inclined to the solar normal. The He II 304 \AA\ moviesshow individual threads, which oscillate and rise to an altitude of about 120Mm with apparent velocities of about 100 km s$^{-1}$, during the rapidevolution phase. Finally, as the flux rope expands into the corona, thefilament disappears by becoming optically thin to undetectable levels. No CMEwas detected by STEREO, only a faint CME was recorded by LASCO at the beginningof the disappearance phase at 02:00 UT, which could be due to partial filamenteruption. Further, STEREO Fe XII 195 \AA\ images showed bright loops beneaththe filament prior to the disappearance phase, suggesting magnetic reconnectionbelow the flux rope.

3D evolution of a filament disappearance event observed by STEREO