  We perform numerical simulations of impulsively generated Alfv\'en waves in
an isolated photospheric flux tube, and explore the propagation of these waves
along such magnetic structure that extends from the photosphere, where these
waves are triggered, to the solar corona, and analyze resulting magnetic
shells. Our model of the solar atmosphere is constructed by adopting the
temperature distribution based on the semi-empirical model and specifying the
curved magnetic field lines that constitute the magnetic flux tube which is
rooted in the solar photosphere. The evolution of the solar atmosphere is
described by 3D, ideal magnetohydrodynamic equations that are numerically
solved by the FLASH code. Our numerical simulations reveal, based on the
physical properties of the multi-shell magnetic twisters and the amount of
energy and momentum associated with them, that these multi-shell magnetic
twisters may be responsible for the observed heating of the lower solar corona
and for the formation of solar wind. Moreover, it is likely that the existence
of these twisters can be verified by high-resolution observations.
