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

TL;DR

This study uses resistive MHD simulations to explore how magnetic resistivity and thermal conduction influence the morphology, velocity, and thermal properties of solar jets resembling Type II spicules and cool coronal jets.

Contribution

It demonstrates that thermal conductivity significantly impacts jet height and temperature, providing new insights into solar jet dynamics and potential plasma diagnostics.

Findings

Thermal conductivity increases jet height and apex temperature.

Magnetic resistivity has minimal effect on jet morphology and velocity.

Jets exchange energy more efficiently at the apex and corona than along their body.

Abstract

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.