  We measure the effects of non-isotropic thermal conduction on generation of
solar chromospheric jets through numerical simulations carried out with the use
of one fluid MHD code MAGNUS. Following the work of Srivastava et al. (2018),
we consider the atmospheric state with a realistic temperature model and
generate the ejection of plasma through a gas pressure driver operating in the
top chromosphere. We consider the magnetic field mimicking a flux tube and
perform parametric studies by varying the magnetic field strength and the
amplitude of the driver. We find that in the case of thermal conduction the
triggered jets exhibit a considerably larger energy and mass fluxes and their
shapes are more collimated and penetrate more the solar corona than for the
ideal MHD equations. Low magnetic fields allow these jets to be more energetic,
and larger magnetic fields decrease the enhancement of mass and energy due to
the inclusion of the thermal conductivity.
