  We show that the coronal heating and the acceleration of the fast solar wind
in the coronal holes are natural consequence of the footpoint fluctuations of
the magnetic fields at the photosphere by one-dimensional, time-dependent, and
nonlinear magnetohydrodynamical simulation with radiative cooling and thermal
conduction. We impose low-frequency (<0.05Hz) transverse photospheric motions,
corresponding to the granulations, with velocity <dv> = 0.7$km/s. In spite of
the attenuation in the chromosphere by the reflection, the sufficient energy of
the generated outgoing Alfven waves transmit into the corona to heat and
accelerate of the plasma by nonlinear dissipation. Our result clearly shows
that the initial cool (10^4K) and static atmosphere is naturally heated up to
10^6K and accelerated to 800km/s, and explain recent SoHO observations and
Interplanetary Scintillation measurements.
