  In this paper, we describe the kinematical and evolutionary properties of the
impulsive cool jets in the solar atmosphere using numerical simulation by
Godunov-type PLUTO code at two different strength of the quiet-Sun magnetic
field (B=56, 112 Gauss). These types of chromospheric jets are originated by
the pressure pulse, which mimics after effects of the localized heating in the
lower solar atmosphere. These jets may be responsible for the transport of mass
and energy in the localized upper atmosphere (i.e., corona). The detection of
the height-time profiles for the jets, originated by imposing the different
pressure pulses, exhibit the asymmetric near parabolic behaviour. This infers
that the upward motion of the jet occurs under the influence of pressure
perturbation. However, its downward motion is not only governed by the
gravitational free fall, but also due to the complex plasma motions near its
base under the effect of counter propagating pulses. Maximum height and
life-time of the jets w.r.t. the strength of the pressure pulse show a linear
increasing trend. This suggests that if the extent of the heating and thus
pressure perturbations will be longer then more longer chromospheric jets can
be triggered from the same location in the chromosphere. For the certain
amplitude of pressure pulse, the strong magnetic field configuration (B=112
Gauss) leads more longer jet compared to the weaker field (B=56 Gauss). This
suggests that the strong magnetic field guides the pressure pulse driven jets
more efficiency towards the higher corona. In conclusion, our model mimics the
properties and evolution of variety of the cool impulsive jets in the
chromosphere (e.g., macrospicules, network jets, isolated repeated cool jets,
confined \& small surges etc).
