  The interstellar medium is characterised by an intricate filamentary network
which exhibits complex structures. These show a variety of different shapes
(e.g. junctions, rings, etc.) deviating strongly from the usually assumed
cylindrical shape. A possible formation mechanism are filament mergers which we
analyse in this study. Indeed, the proximity of filaments in networks suggests
mergers to be rather likely. As the merger has to be faster than the end
dominated collapse of the filament along its major axis we expect three
possible results: (a) The filaments collapse before a merger can happen, (b)
the merged filamentary complex shows already signs of cores at the edges or (c)
the filaments merge into a structure which is not end-dominated. We develop an
analytic formula for the merging and core-formation timescale at the edge and
validate our model via hydrodynamical simulations with the
adaptive-mesh-refinement-code RAMSES. This allows us to predict the outcome of
a filament merger, given different initial conditions which are the initial
distance and the respective line-masses of each filament as well as their
relative velocities.
