  We present the dynamics of two filaments and a C-class flare observed in NOAA
11589 on 2012 October 16. We used the multi-wavelength high-resolution data
from SDO, as well as THEMIS and ARIES ground-based observations. The
observations show that the filaments are progressively converging towards each
other without merging. We find that the filaments have opposite chirality which
may have prevented them from merging. On October 16, a C3.3 class flare
occurred without the eruption of the filaments. According to the standard solar
flare model, after the reconnection, post-flare loops form {\it below} the
erupting filaments whether the eruption fails or not. However, the observations
show the formation of post-flare loops {\it above} the filaments, which is not
consistent with the standard flare model. We analyze the topology of the active
region's magnetic field by computing the quasi-separatrix layers (QSLs) using a
linear force-free field extrapolation. We find a good agreement between the
photospheric footprints of the QSLs and the flare ribbons. We discuss how
slipping or slip-running reconnection at the QSLs may explain the observed
dynamics.
