  Using numerical simulations, we study the effects of thermal conduction and
radiative cooling on the formation and evolution of solar jets with some
macrospicules features. We initially assume that the solar atmosphere is rarely
in equilibrium through energy imbalance. Therefore, we test whether the
background flows resulting from an imbalance between thermal conduction and
radiative cooling influence the jets' behavior. In this particular scenario, we
trigger the formation of the jets by launching a vertical velocity pulse
localized at the upper chromosphere for the following test cases: i) adiabatic
case; ii) thermal conduction case; iii) radiative cooling case; iv) thermal
conduction + radiative cooling case. According to the test results, the
addition of the thermal conduction results in smaller and hotter jets than in
the adiabatic case. On the other hand, the radiative cooling dissipates the jet
after reaching the maximum height ($\approx$ 5.5 Mm), making it shorter and
colder than in the adiabatic and thermal conduction cases. Besides, the flow
generated by the radiative cooling is more substantial than the caused by
thermal conduction. Despite the energy imbalance of the solar atmosphere
background, the simulated jet shows morphological features of macrospicules.
Furthermore, the velocity pulse steepens into a shock that propagates upward
into a solar corona that maintains its initial temperature. The shocks generate
the jets with a quasi-periodical behavior that follows a parabolic path on
time-distance plots consistent with macrospicule jets' observed dynamics.
