  We perform numerical simulations of impulsively generated magnetic swirls in
an isolated flux tube which is rooted in the solar photosphere. These swirls
are triggered by an initial pulse in a horizontal component of the velocity.
The initial pulse is launched either: (a) centrally, within the localized
magnetic flux tube; or (b) off-central, in the ambient medium. The evolution
and dynamics of the flux tube is described by three-dimensional, ideal
magnetohydrodynamic equations. These equations are numerically solved to reveal
that in case (a) dipole-like swirls associated with the fast magnetoacoustic
kink and $m=1$ Alfv\'en waves are generated. In case (b), the fast
magnetoacoustic kink and $m=0$ Alfv\'en modes are excited. In both these cases,
the excited fast magnetoacoustic kink and Alfv\'en waves consist of similar
flow pattern and magnetic shells are also generated with clockwise and
counter-clockwise rotating plasma within them, which can be the proxy of
dipole-shaped chromospheric swirls. The complex dynamics of vortices and wave
perturbations reveals the channelling of sufficient amount of energy to fulfill
energy losses in the chromosphere ($\sim$ 10$^{4}$ W m$^{-1}$) and in the
corona ($\sim$ 10$^{2}$ W m$^{-1}$). Some of these numerical findings are
reminiscent of signatures in recent observational data.
