Rotating Solar Jets in Simulations of Flux Emergence with Thermal Conduction

TL;DR

This paper uses numerical simulations to study coronal jets formed by magnetic flux emergence and reconnection, highlighting the role of thermal conduction and untwisting magnetic fields in producing observed jet features.

Contribution

It introduces a simulation model that incorporates thermal conduction to replicate observed coronal jet dynamics and emission, emphasizing the importance of untwisting magnetic fields.

Findings

Simulated jets exhibit rotational motion of about 20 km/s.

Thermal conduction allows qualitative comparison with observed emissions.

Untwisting magnetic fields drive plasma outflows and jet spinning.

Abstract

We study the formation of coronal jets through numerical simulation of the emergence of a twisted magnetic flux rope into a pre-existing open magnetic field. Reconnection inside the emerging flux rope in addition to that between the emerging and pre-existing fields give rise to the violent eruption studied. The simulated event closely resembles the coronal jets ubiquitously observed by Hinode/XRT and demonstrates that heated plasma is driven into the extended atmosphere above. Thermal conduction implemented in the model allows us to qualitatively compare simulated and observed emission from such events. We find that untwisting field lines after the reconnection drive spinning outflows of plasma in the jet column. The Poynting flux in the simulated jet is dominated by the untwisting motions of the magnetic fields loaded with high-density plasma. The simulated jet is comprised of spires of untwisting field that are loaded with a mixture of cold and hot plasma and exhibit rotational motion of order 20 km/s and match contemporary observations.