  Context. The magnetic Kelvin-Helmholtz instability (KHI) has been proposed as
a means of generating magnetohy- drodynamic turbulence and encouraging wave
energy dissipation in the solar corona, particularly within transversely
oscillating loops. Aims. Our goal is to determine whether the KHI encourages
magnetic reconnection in oscillating flux tubes in the solar corona. This will
establish whether the instability enhances the dissipation rate of energy
stored in the magnetic field. Methods. We conducted a series of
three-dimensional magnetohydrodynamic simulations of the KHI excited by an
oscillating velocity shear. We investigated the effects of numerical
resolution, field line length, and background currents on the growth rate of
the KHI and on the subsequent rate of magnetic reconnection. Results. The KHI
is able to trigger magnetic reconnection in all cases, with the highest rates
occurring during the initial growth phase. Reconnection is found to occur
preferentially along the boundaries of Kelvin-Helmholtz vortices, where the
shear in the velocity and magnetic fields is greatest. The estimated rate of
reconnection is found to be lowest in simulations where the KHI growth rate is
reduced. For example, this is the case for shorter field lines or due to shear
in the background field. Conclusions. In non-ideal regimes, the onset of the
instability causes the local reconnection of magnetic field lines and enhances
the rate of coronal wave heating. However, we found that if the equilibrium
magnetic field is sheared across the Kelvin-Helmholtz mixing layer, the
instability does not significantly enhance the rate of reconnection of the
background field, despite the free energy associated with the non-potential
field.
