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Using numerical simulations, we study the effects of magnetic resistivity andthermal conductivity in the dynamics and properties of solar jets withcharacteristics of Type II spicules and cool coronal jets. The dynamicevolution of the jets is governed by the resistive MHD equations with thermalconduction along the magnetic field lines on a 2.5D slice. The magnetic fieldconfiguration consists of two symmetric neighboring loops with oppositepolarity, used to support reconnection and followed by the plasma jetformation. In total 10 simulations were carried out with different values ofresistivity and thermal conductivity, that produce jets with differentmorphological and thermal properties we quantify. We find that an increase inmagnetic resistivity does not produce significant effects on the morphology,velocity and temperature of the jets. However, thermal conductivity affectsboth temperature and morphology of the jets. In particular, thermalconductivity causes jets to reach greater heights and increases the temperatureof the jet-apex. Also, heat flux maps indicate the jet-apex and coronainterchange energy more efficiently than the body of the jet. These resultscould potentially open a new avenue for plasma diagnostics in the Sun'satmosphere.

Spicule jets in the solar atmosphere modeled with resistive MHD and thermal conduction