  We present results of three-dimensional numerical simulations of
magnetohydrodynamic (MHD) wave propagation in a solar magnetic flux tube. Our
study aims at understanding the properties of a range of MHD wave modes
generated by different photospheric motions. We consider two scenarios observed
in the lower solar photosphere, namely, granular buffeting and vortex-like
motion, among the simplest mechanism for the generation of waves within a
strong, localized magnetic flux concentration. We show that granular buffeting
is likely to generate stronger slow and fast magnetoacoustic waves as compared
to swirly motions. Correspondingly, the energy flux transported differs as a
result of the driving motions. We also demonstrate that the waves generated by
granular buffeting are likely to manifest in stronger emission in the
chromospheric network. We argue that different mechanisms of wave generation
are active during the evolution of a magnetic element in the intergranular
lane, resulting in temporally varying emission at chromospheric heights.
