  This work is an extension of Kaghashvili [1999] where ion-cyclotron wave
dissipation channel for Alfv\'en waves was discussed. While our earlier study
dealt with the mode coupling in the commonly discussed sense, here we study
changes in the initial waveform due to interaction of the initial driver
Alfv\'en wave and the plasma inhomogeneity, which are implicitly present in the
equations, but were not elaborated in Kaghashvili [1999]. Using a cold plasma
approximation, we show how high frequency waves (higher than the initial driver
Alfv\'en wave frequency) are generated in the inhomogeneous solar plasma flow.
The generation of the high frequency forward and backward propagating modified
fast magnetosonic/whistler waves as well as the generation of the driven
Alfv\'en waves is discussed in the solar atmosphere. The generated high
frequency waves have a shorter dissipation timescale, and they can also
resonant interact with particles using both the normal cyclotron and anomalous
cyclotron interaction channels. These waves can also be important in space,
Earths magnetosphere, the ionosphere, and laboratory plasma processes.
