Solar flares are one of the most energetic phenomena in the solar system. During these events, magnetic energy is converted into particle acceleration and heating via magnetic reconnection. In a recent 3D model of solar flares (Aulanier+ 2013), lines of magnetic field undergo so-called slipping reconnection, which takes place in both sub- and super- Alfvénic regimes. Slow sub- Alfvénic regime of slipping reconnection has already been observed (e.g. Dudík+ 2014, 2016), but observations of super- Alfvénic regime have not yet been published. We report on first observations of super- Alfvénic regime of magnetic slipping reconnection in an eruption of a quiescent filament observed on August 31 2012.