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The solar wind emanates from the hot and tenuous solar corona. Earlierstudies using 1.5 dimensional simulations show that Alfv\'{e}n waves generatedin the photosphere play an important role in coronal heating through theprocess of non-linear mode conversion. In order to understand the physics ofcoronal heating and solar wind acceleration together, it is important toconsider the regions from photosphere to interplanetary space as a singlesystem. We performed 2.5 dimensional, self-consistent magnetohydrodynamicsimulations, covering from the photosphere to the interplanetary space for thefirst time. We carefully set up the grid points with spherical coordinate totreat the Alfv\'{e}n waves in the atmosphere with huge density contrast, andsuccessfully simulate the solar wind streaming out from the hot solar corona asa result of the surface convective motion. The footpoint motion excitesAlfv\'{e}n waves along an open magnetic flux tube, and these waves travelingupwards in the non-uniform medium undergo wave reflection, nonlinear modeconversion from Alfv\'{e}n mode to slow mode, and turbulent cascade. Theseprocesses leads to the dissipation of Alfv\'{e}n waves and acceleration of thesolar wind. It is found that the shock heating by the dissipation of the slowmode wave plays a fundamental role in the coronal heating process whereas theturbulent cascade and shock heating drive the solar wind.

Connecting the Sun and the Solar Wind: The First 2.5 Dimensional Self-consistent MHD Simulation under the Alfv\'en Wave Scenario