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We have performed a 2.5 dimensional magnetohydrodynamic simulation thatresolves the propagation and dissipation of Alfven waves in the solaratmosphere. Alfvenic fluctuations are introduced on the bottom boundary of theextremely large simulation box that ranges from the photosphere to far abovethe solar wind acceleration region. Our model is ab initio in the sense that nocorona and no wind are assumed initially.The numerical experiment reveals thequasi-steady solution that has the transition from the cool to the hotatmosphere and the emergence of the high speed wind. The global structure ofthe resulting hot wind solution fairly well agree with the coronal and thesolar wind structure inferred from observations. The purpose of this study isto complement the previous paper by Matsumoto & Suzuki (2012) and describe themore detailed results and the analysis method. These results include thedynamics of the transition region and the more precisely measured heating ratein the atmosphere. Particularly, the spatial distribution of the heating ratehelps us to interpret the actual heating mechanisms in the numericalsimulation.Our estimation method of heating rate turned out to be a goodmeasure for dissipation of Alfven waves and low beta fast waves.

Connecting the Sun and the Solar Wind: The Self-consistent Transition of Heating Mechanisms