In this work, we perform 3D numerical simulations applicable to the lower solar atmosphere which implement Alfven vortices as photospheric drivers. These drivers are used to excite MHD waves in an axially symmetric, 3D magnetic flux tube embedded in a gravitationally and magnetically sratified realistic model solar atmosphere. Analysis is carried out of how azimuthal wavenumber, m, of the driver is varied and the resulting perturbations are discussed.

It was found that motions with greater azimuthal wavenumber persisted higher into the atmosphere. These motions also generated clearer structuring of density enhancements and reductions.