  We analyze the observations of EUV loop evolution associated with the
filament eruption located at the border of an active region. The event
SOL2013-03-16T14:00 was observed with a large difference of view point by the
Solar Dynamics Observatory and Solar Terrestrial Relations Observatory --A
spacecraft. The filament height is fitted with the sum of a linear and
exponential function. These two phases point to different physical mechanisms
such as: tether-cutting reconnection and a magnetic instability. While no X-ray
emission is reported, this event presents the classical eruption features like:
separation of double ribbons and the growth of flare loops. We report the
migration of the southern foot of the erupting filament flux rope due to the
interchange reconnection with encountered magnetic loops of a neighbouring AR.
Parallel to the erupting filament, a stable filament remains in the core of
active region. The specificity of this eruption is that coronal loops, located
above 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 at
the eruption onset. Both contraction and expansion phases last around 20 min.
The main difference with previous cases is that the PIL bent about 180 deg
around the end of the erupting filament because the magnetic configuration is
at least tri-polar. These observations are challenging for models which
interpreted previous cases of loop contraction within a bipolar configuration.
New simulations are required to broaden the complexity of the configurations
studied.
