  Identifying the underlying mechanisms behind the excitation of transverse
oscillations in coronal loops is essential for their role as diagnostic tools
in coronal seismology and their potential use as wave heating mechanisms of the
solar corona. In this paper, we explore the concept of these transverse
oscillations being excited through a self-sustaining process, caused by
Alfv\'{e}nic vortex shedding from strong background flows interacting with
coronal loops. We show for the first time in 3D simulations that vortex
shedding can generate transverse oscillations in coronal loops, in the
direction perpendicular to the flow due to periodic "pushing" by the vortices.
By plotting the power spectral density we identify the excited frequencies of
these oscillations. We see that these frequencies are dependent both on the
speed of the flow, as well as the characteristics of the oscillating loop.
This, in addition to the fact that the background flow is constant and not
periodic, makes us treat this as a self-oscillating process. Finally, the
amplitudes of the excited oscillations are near constant in amplitude, and are
comparable with the observations of decay-less oscillations. This makes the
mechanism under consideration a possible interpretation of these undamped waves
in coronal loops.
