An M Dwarf’s Chromosphere, Corona, and Wind Connection via Nonlinear Alfvén Waves

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