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Alfv\'en waves are responsible for the transfer of magnetic energy in themagnetized plasma. They are involved in heating solar atmosphere and drivingsolar wind through various nonlinear processes. Since the magnetic fieldconfigurations directly affect the nonlinearity of Alfv\'en waves, it isimportant to investigate how they relate to the solar atmosphere and windstructure through the nonlinear propagation of Alfv\'en waves. In this study,we carried out the one-dimensional magnetohydrodynamic simulations to realizethe above relation. The results show that when the nonlinearity of Alfv\'enwaves in the chromosphere exceeds a critical value, the dynamics of the solarchromosphere (e.g., spicule) and the mass loss rate of solar wind tend to beindependent of the energy input from the photosphere. In a situation where theAlfv\'en waves are highly nonlinear, the strong shear torsional flow generatedin the chromosphere ``fractures'' the magnetic flux tube. This corresponds tothe formation of chromospheric intermediate shocks, which limit thetransmission of the Poynting flux into the corona by Alfv\'en waves and alsoinhibits the propagation of chromospheric slow shock.

Energy Transfer by Nonlinear Alfv\'en Waves in the Solar Chromosphere,  and Its Effect on Spicule Dynamics, Coronal Heating, and Solar Wind  Acceleration