  Using numerical simulations, we study the effects of magnetic resistivity and
thermal conductivity in the dynamics and properties of solar jets with
characteristics of Type II spicules and cool coronal jets. The dynamic
evolution of the jets is governed by the resistive MHD equations with thermal
conduction along the magnetic field lines on a 2.5D slice. The magnetic field
configuration consists of two symmetric neighboring loops with opposite
polarity, used to support reconnection and followed by the plasma jet
formation. In total 10 simulations were carried out with different values of
resistivity and thermal conductivity, that produce jets with different
morphological and thermal properties we quantify. We find that an increase in
magnetic resistivity does not produce significant effects on the morphology,
velocity and temperature of the jets. However, thermal conductivity affects
both temperature and morphology of the jets. In particular, thermal
conductivity causes jets to reach greater heights and increases the temperature
of the jet-apex. Also, heat flux maps indicate the jet-apex and corona
interchange energy more efficiently than the body of the jet. These results
could potentially open a new avenue for plasma diagnostics in the Sun's
atmosphere.
