  Using simulated data-driven three-dimensional resistive MHD simulations of
the solar atmosphere, we show that magnetic reconnection can be responsible of
the formation of jets with characteristic of Type II spicules. For this, we
numerically model the photosphere-corona region using the C7 equilibrium
atmosphere model. The initial magnetic configuration is a 3D potential magnetic
field, extrapolated up to the solar corona region from a dynamic realistic
simulation of solar photospheric magnetoconvection model which is mimicking
quiet-Sun. In this case we consider a uniform and constant value of the
magnetic resistivity of $12.56 ~\Omega~{\rm m}$. We have found that formation
of the jets depends on the Lorentz force, which helps to accelerate the plasma
upwards. Analyzing various properties of the jet dynamics, we found that the
jet structure shows Doppler shift near to regions with high vorticity. The
morphology, upward velocity, covering a range up to 100 $\rm km$ $\rm s^{-1}$,
and life-time of the estructure, bigger than 100 ${\rm s}$, are similar to
those expected for Type II spicules.
