  In recent years, omni-present transverse waves have been observed in all
layers of the solar atmosphere. Coronal loops are often modeled as a collection
of individual strands, in order to explain their thermal behaviour and
appearance. We perform 3D ideal MHD simulations to study the effect of a
continuous small amplitude transverse footpoint driving on the internal
structure of a coronal loop composed of strands. The output is also converted
to synthetic images, corresponding to the AIA 171 A and 193 A passbands, using
FoMo. We show that the multi-stranded loop ceases to exist in the traditional
sense of the word, because the plasma is efficiently mixed perpendicularly to
the magnetic field, with the Kelvin-Helmholtz instability acting as the main
mechanism. The final product of our simulation is mixed loop with density
structures on a large range of scales, resembling a power-law. Thus,
multi-stranded loops are unstable to driving by transverse waves, and this
raises a strong doubt on the usability and applicability of coronal loop models
consisting of independent strands.
