Evolution of a Current Sheet in a Solar Flare

TL;DR

This paper presents multi-wavelength observations of a solar flare, focusing on the evolution of a current sheet and magnetic reconnection processes, providing detailed physical properties and dynamics of the event.

Contribution

It offers new insights into the physical characteristics and evolution of current sheets during solar flares through detailed observational analysis.

Findings

Evidence of magnetic reconnection during the flare.

Measured physical properties of the current-sheet-like structure.

Observed pre-flare EUV emission increase and coronal dimming.

Abstract

We report multi-wavelength and multi-viewpoint observations of a solar eruptive event which involves loop-loop interactions. During a C2.0 flare, motions associated with inflowing and outflowing plasma provide evidence for ongoing magnetic reconnection. The flare loop top and a rising "concave-up" feature are connected by a current-sheet-like structure (CSLS). The physical properties (thickness, length, temperature, and density) of the CSLS are evaluated. In regions adjacent to the CSLS, the EUV emission (characteristic temperature at 1.6 MK) begins to increase more than ten minutes prior to the onset of the flare, and steeply decreases during the decay phase. The reduction of the emission resembles that expected from coronal dimming. The dynamics of this event imply a magnetic reconnection rate in the range 0.01 -- 0.05.