Fan-shaped jets in three dimensional reconnection simulation as a model of ubiquitous solar jets

TL;DR

This paper presents a 3D simulation model of magnetic reconnection that explains the formation and movement of ubiquitous solar jets along guide field lines, enhancing understanding of small-scale solar phenomena.

Contribution

It introduces a novel 3D reconnection model with a strong guide field that accounts for the observed behavior of solar jets.

Findings

Jets move along guide field lines in the simulation

The model explains the formation of ubiquitous solar jets

Provides new insights into astrophysical magnetic reconnection

Abstract

Magnetic reconnection is a fundamental process in space and astrophysical plasmas in which oppositely directed magnetic fields changes its connectivity and eventually converts its energy into kinetic and thermal energy of the plasma. Recently, ubiquitous jets (for example, chromospheric anemone jets, penumbral microjets, umbral light bridge jets) have been observed by Solar Optical Telescope on board the satellite Hinode. These tiny and frequently occurring jets are considered to be a possible evidence of small-scale ubiquitous reconnection in the solar atmosphere. However, the details of three dimensional magnetic configuration are still not very clear. Here we propose a new model based on three dimensional simulations of magnetic reconnection using a typical current sheet magnetic configuration with a strong guide field. The most interesting feature is that the jets produced by the reconnection eventually move along the guide field lines. This model provides a fresh understanding of newly discovered ubiquitous jets and moreover a new observational basis for the theory of astrophysical magnetic reconnection.