We show that the coronal heating and the fast solar wind acceleration in the coronal holes are natural consequence of the footpoint fluctuations of the magnetic fields at the photosphere , by performing one-dimensional magnetohydrodynamical simulation with radiative cooling and thermal conduction .
We initially set up a static open flux tube with temperature 10 ^ { 4 } K rooted at the photosphere .
We impose transverse photospheric motions corresponding to the granulations with velocity \langle dv _ { \perp } \rangle = 0.7 km/s and period between 20 seconds and 30 minutes , which generate outgoing Alfvén waves .
We self-consistently treat these waves and the plasma heating .
After attenuation in the chromosphere by \simeq 85 % of the initial energy flux , the outgoing Alfvén waves enter the corona and contribute to the heating and acceleration of the plasma mainly by the nonlinear generation of the compressive waves and shocks .
Our result clearly shows that the initial cool and static atmosphere is naturally heated up to 10 ^ { 6 } K and accelerated to \simeq 800 km/s . The mpeg movie for fig.1 is available at

http : //www-tap.scphys.kyoto-u.ac.jp/~stakeru/research/suzuki_200506.mpg