Chromospheric Magnetic Reconnection caused by Photospheric Flux Emergence: Implications for Jet-like Events Formation

TL;DR

This study uses a resistive MHD model to explore how magnetic reconnection in the chromosphere, influenced by photospheric flux emergence, can produce jet-like events with properties matching observations.

Contribution

It demonstrates how environmental factors like magnetic field strength and plasma density affect jet temperatures and velocities during chromospheric magnetic reconnection.

Findings

Jets reach up to 600,000 K in high magnetic field environments.

Jet velocities can be as high as 130 km/s under certain conditions.

Lower magnetic fields produce cooler, slower jets.

Abstract

Magnetic reconnection in the low atmosphere, e.g. chromosphere, is investigated in various physical environments. Its implications for the origination of explosive events (small--scale jets) are discussed. A 2.5-dimensional resistive magnetohydrodynamic (MHD) model in Cartesian coordinates is used. It is found that the temperature and velocity of the outflow jets as a result of magnetic reconnection are strongly dependent on the physical environments, e.g. the magnitude of the magnetic field strength and the plasma density. If the magnetic field strength is weak and the density is high, the temperature of the jets is very low (~10,000 K) as well as its velocity (~40 km/s). However, if environments with stronger magnetic field strength (20 G) and smaller density (electron density Ne=2x10^{10} cm^{-3}) are considered, the outflow jets reach higher temperatures of up to 600,000 K and a line-of-sight velocity of up to 130 km/s which is comparable with the observational values of jet-like events.