Thermal conduction effects on formation of chromospheric solar tadpole-like jets

TL;DR

This study investigates how non-isotropic thermal conduction influences the formation and properties of chromospheric solar jets using numerical MHD simulations, revealing enhanced jet energy, mass flux, and collimation.

Contribution

It provides the first detailed analysis of thermal conduction effects on solar chromospheric jets within a realistic atmospheric model using parametric MHD simulations.

Findings

Thermal conduction increases jet energy and mass flux.

Jets with thermal conduction are more collimated and penetrate deeper into the corona.

Lower magnetic fields lead to more energetic jets with thermal conduction.

Abstract

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.