  We investigate coronal heating and acceleration of the high- and low-speed
solar wind in the open field region by dissipation of fast and slow
magnetohydrodynamical (MHD) waves through MHD shocks. Linearly polarized
\Alfven (fast MHD) waves and acoustic (slow MHD) waves travelling upwardly
along with a magnetic field line eventually form fast switch-on shock trains
and hydrodynamical shock trains (N-waves) respectively to heat and accelerate
the plasma. We determine one dimensional structure of the corona from the
bottom of the transition region (TR) to 1AU under the steady-state condition by
solving evolutionary equations for the shock amplitudes simultaneously with the
momentum and proton/electron energy equations. Our model reproduces the overall
trend of the high-speed wind from the polar holes and the low-speed wind from
the mid- to low-latitude streamer except the observed hot corona in the
streamer. The heating from the slow waves is effective in the low corona to
increase the density there, and plays an important role in the formation of the
dense low-speed wind. On the other hand, the fast waves can carry a sizable
energy to the upper level to heat the outer corona and accelerate the
high-speed wind effectively. We also study dependency on field strength, $B_0$,
at the bottom of the TR and non-radial expansion of a flow tube, $f_{\rm max}$,
to find that large $B_0/f_{\rm max}\gtrsim 2$ but small $B_0\simeq 2$G are
favorable for the high-speed wind and that small $B_0/f_{\rm max}\simeq 1$ is
required for the low-speed wind.
