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We analyze the observations of EUV loop evolution associated with thefilament eruption located at the border of an active region. The eventSOL2013-03-16T14:00 was observed with a large difference of view point by theSolar Dynamics Observatory and Solar Terrestrial Relations Observatory --Aspacecraft. The filament height is fitted with the sum of a linear andexponential function. These two phases point to different physical mechanismssuch as: tether-cutting reconnection and a magnetic instability. While no X-rayemission is reported, this event presents the classical eruption features like:separation of double ribbons and the growth of flare loops. We report themigration of the southern foot of the erupting filament flux rope due to theinterchange reconnection with encountered magnetic loops of a neighbouring AR.Parallel to the erupting filament, a stable filament remains in the core ofactive region. The specificity of this eruption is that coronal loops, locatedabove the nearly joining ends of the two filaments, first contract in phase,then expand and reach a new stable configuration close to the one present atthe eruption onset. Both contraction and expansion phases last around 20 min.The main difference with previous cases is that the PIL bent about 180 degaround the end of the erupting filament because the magnetic configuration isat least tri-polar. These observations are challenging for models whichinterpreted previous cases of loop contraction within a bipolar configuration.New simulations are required to broaden the complexity of the configurationsstudied.

Filament Eruption Driving EUV Loop Contraction then Expansion above a Stable Filament