抄録
Solar wind is the outflow of hot coronal plasma. Magnetohydrodynamical (MHD) wave and turbulence play an essential role in driving solar wind as well as stellar winds from solar-type stars. The sun, and in general,low-mass stars possess surface convective zones. Various modes of waves are excited from the stellar surfaces due to the convective motions, and these waves dissipate through various nonlinear processes such as turbulent cascade and the generation of compressive waves. As a result, the kinetic energy of the surface convection in the interior is transported to the upper atmosphere, which drives the wind. In this paper, we discuss these consecutive processes from both theoretical and observational viewpoints, and review our recent results of MHD simulations.
