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