  In the solar atmosphere, jets are prevalent and they are significant for the
mass and energy transport. Here we conduct numerical simulations to investigate
the mass and energy contributions of the recently observed high-speed jets to
the solar wind. With a one-dimensional hydrodynamic solar wind model, the
time-dependent pulses are imposed at the bottom to simulate the jets. The
simulation results show that without other energy source, the injected plasmas
are accelerated effectively to be a transonic wind with a substantial mass
flux. The rapid acceleration occurs close to the Sun, and the resulting
asymptotic speed, number density at 0.3 AU, as well as mass flux normalized to
1 AU are compatible with in situ observations. As a result of the high speed,
the imposed pulses generate a train of shocks traveling upward. By tracing the
motions of the injected plasma, it is found that these shocks heat and
accelerate the injected plasmas successively step by step to push them upward
and eventually allow them to escape. The parametric studies show that
increasing the speed of the imposed pulses or their temperature gives a
considerably faster, and hotter solar wind, while increasing their number
density or decreasing their recurring period only bring a denser solar wind.
These studies provide a possibility that the ubiquitous high-speed jets are a
substantial mass and energy contributions to the solar wind.
