  Using a three-dimensional compressible magnetohydrodynamic (MHD) simulation,
we have reproduced the fast solar wind in a direct and self-consistent manner,
based on the wave/turbulence driven scenario. As a natural consequence of
Alfvenic perturbations at its base, highly compressional and turbulent
fluctuations are generated, leading to heating and acceleration of the solar
wind. The analysis of power spectra and structure functions reveals that the
turbulence is characterized by its imbalanced (in the sense of outward Alfvenic
fluctuations) and anisotropic nature. The density fluctuation originates from
the parametric decay instability of outwardly propagating Alfven waves and
plays a significant role in the Alfven wave reflection that triggers
turbulence. Our conclusion is that the fast solar wind is heated and
accelerated by compressible MHD turbulence driven by parametric decay
instability and resultant Alfven wave reflection.
