  In this talk we introduce our recent results of global 1D MHD simulations for
the acceleration of solar and stellar winds. We impose transverse photospheric
motions corresponding to the granulations, which generate outgoing Alfven
waves. The Alfven waves effectively dissipate by 3-wave coupling and direct
mode conversion to compressive waves in density-stratified atmosphere. We show
that the coronal heating and the solar wind acceleration in the open magnetic
field regions are natural consequence of the footpoint fluctuations of the
magnetic fields at the surface (photosphere). We also discuss winds from red
giant stars driven by \Alfven waves, focusing on different aspects from the
solar wind. We show that red giants wind are highly structured with
intermittent magnetized hot bubbles embedded in cool chromospheric material.
