  In this paper, we show a "proof of concept" of the heating mechanism of the
solar chromosphere due to wave dissipation caused by the effects of partial
ionization. Numerical modeling of non-linear wave propagation in a magnetic
flux tube, embedded in the solar atmosphere, is performed by solving a system
of single-fluid quasi-MHD equations, which take into account the ambipolar term
from the generalized Ohm's law. It is shown that perturbations caused by
magnetic waves can be effectively dissipated due to ambipolar diffusion. The
energy input by this mechanism is continuous and shown to be more efficient
than dissipation of static currents, ultimately leading to chromospheric
temperature increase in magnetic structures.
