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Vortex motions are frequently observed on the solar photosphere. Thesemotions may play a key role in the transport of energy and momentum from thelower atmosphere into the upper solar atmosphere, contributing to coronalheating. The lower solar atmosphere also consists of complex networks of fluxtubes that expand and merge throughout the chromosphere and upper atmosphere.We perform numerical simulations to investigate the behaviour of vortex drivenwaves propagating in a pair of such flux tubes in a non-force-free equilibriumwith a realistically modelled solar atmosphere. The two flux tubes areindependently perturbed at their footpoints by counter-rotating vortex motions.When the flux tubes merge, the vortex motions interact both linearly andnonlinearly. The linear interactions generate many small-scale transientmagnetic substructures due to the magnetic stress imposed by the vortexmotions. Thus, an initially monolithic tube is separated into a complexmulti-threaded tube due to the photospheric vortex motions. The waveinteractions also drive a superposition that increases in amplitude until itexceeds the local Mach number and produces shocks that propagate upwards withspeeds of approximately $ 50$ km s$^{-1}$. The shocks act as conduitstransporting momentum and energy upwards, and heating the local plasma by morethan an order of magnitude, with peak temperature approximately $60,000$ K.Therefore, we present a new mechanism for the generation of magnetic waveguidesfrom the lower solar atmosphere to the solar corona. This wave guide appears asthe result of interacting perturbations in neighbouring flux tubes. Thus, theinteractions of photospheric vortex motions is a potentially significantmechanism for energy transfer from the lower to upper solar atmosphere.

Magnetic shocks and substructures excited by torsional Alfv\'en wave interactions in merging expanding flux tubes