  M dwarf's atmosphere is expected to be highly magnetized. The magnetic energy
can be responsible for heating the stellar chromosphere and corona, and driving
the stellar wind. The nonlinear propagation of Alfv\'en wave is the promising
mechanism for both heating stellar atmosphere and driving stellar wind. Based
on this Alfv\'en wave scenario, we carried out the one-dimensional compressive
magnetohydrodynamic (MHD) simulation to reproduce the stellar atmospheres and
winds of TRAPPIST-1, Proxima Centauri, YZ CMi, AD Leo, AX Mic, as well as the
Sun. The nonlinear propagation of Alfv\'en wave from the stellar photosphere to
chromosphere, corona, and interplanetary space is directly resolved in our
study. The simulation result particularly shows that the slow shock generated
through the nonlinear mode coupling of Alfv\'en wave is crucially involved in
both dynamics of stellar chromosphere (stellar spicule) and stellar wind
acceleration. Our parameter survey further revealed the following general
trends of physical quantities of stellar atmosphere and wind. (1) The M dwarfs'
coronae tend to be cooler and denser than solar corona. (2) M dwarfs' stellar
winds can be characterized with relatively faster velocity and much smaller
mass-loss rate compared to those of solar wind. The physical mechanisms behind
these tendencies are clarified in this paper, where the stronger stratification
of M dwarf's atmosphere and relatively smaller Alfv\'en wave energy input from
the M dwarf's photosphere are remarkable.
