  M dwarf's atmosphere and wind is expected to be highly magnetized. The
nonlinear propagation of Alfv\'en wave could play a key role in both heating
the stellar atmosphere and driving the stellar wind. Along this Alfv\'en wave
scenario, we carried out the one-dimensional compressive magnetohydrodynamic
(MHD) simulation about the nonlinear propagation of Alfv\'en wave from the M
dwarf's photosphere, chromosphere to the corona and interplanetary space. Based
on the simulation results, we develop the semi-empirical method describing the
solar and M dwarf's coronal temperature, stellar wind velocity, and wind's mass
loss rate. We find that M dwarfs' coronae tend to be cooler than solar corona,
and that M dwarfs' stellar winds would be characterized with faster velocity
and much smaller mass loss rate compared to those of the solar wind.
