Three-dimensional Magnetohydrodynamic Simulation of the Formation of Solar Chromospheric Jets with Twisted Magnetic Field Lines

TL;DR

This study uses 3D MHD simulations to model the formation of solar chromospheric jets with twisted magnetic fields, revealing their dynamics, structure, and relation to solar spicules.

Contribution

It introduces a realistic 3D simulation approach incorporating detailed radiative transfer and thermodynamics to study chromospheric jet formation.

Findings

Jets reach heights of 10-11 Mm and last 8-10 minutes.

Magnetic field lines are highly entangled, driving jets via Lorentz force.

Jets form clusters with fine strands, resembling solar spicules.

Abstract

This paper presents a three-dimensional simulation of chromospheric jets with twisted magnetic field lines. Detailed treatments of the photospheric radiative transfer and the equation of states allow us to model realistic thermal convection near the solar surface, which excites various MHD waves and produces chromospheric jets in the simulation. A tall chromospheric jet with a maximum height of 10--11 Mm and lifetime of 8--10 min is formed above a strong magnetic field concentration. The magnetic field lines are strongly entangled in the chromosphere, which helps the chromospheric jet to be driven by the Lorentz force. The jet exhibits oscillatory motion as a natural consequence of its generation mechanism. We also find that the produced chromospheric jet forms a cluster with a diameter of several Mm with finer strands. These results imply a close relationship between the simulated jet and solar spicules.