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Oscillatory reconnection is a process that has been suggested to underlieseveral solar and stellar phenomena, and is likely to play an important role intransient events such as flares. Quasi-periodic pulsations (QPPs) in flareemissions may be a manifestation of oscillatory reconnection, but theunderlying mechanisms remain uncertain. In this paper, we present 2Dmagnetohydrodynamic (MHD) simulations of two current-carrying magnetic fluxropes with an out-of-plane magnetic field undergoing oscillatory reconnectionin which the two flux ropes merge into a single flux rope. We find thatoscillatory reconnection can occur intrinsically without an externaloscillatory driver during flux rope coalescence, which may occur both duringlarge-scale coronal loop interactions and the merging of plasmoids infragmented current sheets. Furthermore, we demonstrate that radiallypropagating non-linear waves are produced in the aftermath of flux ropecoalescence, due to the post-reconnection oscillations of the merged flux rope.The behaviour of these waves is found to be almost independent of the initialout-of-plane magnetic field. It is estimated that the waves emitted throughmerging coronal loops and merging plasmoids in loop-top current sheets wouldhave a typical phase speed of 90 km/s and 900 km/s respectively. It is possiblethat the properties of the waves emitted during flux rope coalescence could beused as a diagnostic tool to determine physical parameters within a coalescingregion.

Oscillatory reconnection and waves driven by merging magnetic flux ropes in solar flares