  Understanding the mechanism(s) of the solar wind acceleration is important in
astrophysics and geophysics. A promising model of the solar wind acceleration
is known as the wave/turbulence-driven (WTD) model, in which Alfv\'en waves
feed energy to the solar wind. In this study, we tested the WTD model with
global measurement of wind speed from interplanetary scintillation (IPS)
observations. For Carrington rotations in minimal and maximal activity phases,
we selected field lines calculated by the potential-field source-surface method
in high- and mid-latitudes and compared the simulated and observed wind
velocities. The simulation was performed in a self-consistent manner by solving
the magnetohydrodynamic equations from the photosphere to the solar wind. In
high-latitude regions, the simulated solar wind velocity agrees better with the
IPS observation than with the classical Wang--Sheeley empirical estimation,
both in maximal and minimal activity phases. In mid-latitude regions, the
agreement worsens, possibly because of the inaccuracy of the WTD model and/or
the magnetic-field extrapolation. Our results indicate that the high-latitude
solar wind is likely to be driven by waves and turbulence, and that the
physics-based prediction of the solar wind velocity is highly feasible with an
improved magnetic-field extrapolation.
