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M dwarf's atmosphere is expected to be highly magnetized. The magnetic energycan be responsible for heating the stellar chromosphere and corona, and drivingthe stellar wind. The nonlinear propagation of Alfv\'en wave is the promisingmechanism for both heating stellar atmosphere and driving stellar wind. Basedon this Alfv\'en wave scenario, we carried out the one-dimensional compressivemagnetohydrodynamic (MHD) simulation to reproduce the stellar atmospheres andwinds of TRAPPIST-1, Proxima Centauri, YZ CMi, AD Leo, AX Mic, as well as theSun. The nonlinear propagation of Alfv\'en wave from the stellar photosphere tochromosphere, corona, and interplanetary space is directly resolved in ourstudy. The simulation result particularly shows that the slow shock generatedthrough the nonlinear mode coupling of Alfv\'en wave is crucially involved inboth dynamics of stellar chromosphere (stellar spicule) and stellar windacceleration. Our parameter survey further revealed the following generaltrends 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' stellarwinds can be characterized with relatively faster velocity and much smallermass-loss rate compared to those of solar wind. The physical mechanisms behindthese tendencies are clarified in this paper, where the stronger stratificationof M dwarf's atmosphere and relatively smaller Alfv\'en wave energy input fromthe M dwarf's photosphere are remarkable.

M-dwarf's Chromosphere, Corona and Wind Connection via the Nonlinear Alfv\'en Wave