Statistical Properties of Ribbon Evolution and Reconnection Electric Fields in Eruptive and Confined Flares

TL;DR

This study statistically analyzes the evolution of chromospheric ribbons and reconnection electric fields in 50 flares, revealing differences between confined and eruptive flares and their relation to flare strength and CMEs.

Contribution

It provides a comprehensive statistical comparison of ribbon evolution and electric fields in confined versus eruptive flares, highlighting key differences and correlations.

Findings

Eruptive flares show larger ribbon separation and higher velocities.

Ribbon separation correlates with GOES flux in eruptive flares.

Stronger electric fields are associated with more powerful flares and faster CMEs.

Abstract

A statistical study of the chromospheric ribbon evolution in H$\alpha$ two-ribbon flares is performed. The data set consists of 50 confined ($62\,\%$) and eruptive ($38\,\%$) flares that occurred from June 2000 to June 2015. The flares are selected homogeneously over the H$\alpha$ and $\textit{GOES}$ (Geostationary Operational Environmental Satellite) classes, with an emphasis on including powerful confined flares and weak eruptive flares. H$\alpha$ filtergrams from Kanzelh\"ohe Observatory in combination with $\textit{MDI}$ (Michelson Doppler Imager) and $\textit{HMI}$ (Helioseismic and Magnetic Imager) magnetograms are used to derive the ribbon separation, the ribbon-separation velocity, the magnetic-field strength, and the reconnection electric field. We find that eruptive flares reveal statistically larger ribbon separation and higher ribbon-separation velocities than confined flares. In addition, the ribbon separation of eruptive flares correlates with the GOES SXR flux, whereas no clear dependence was found for confined flares. The maximum ribbon-separation velocity is not correlated with the GOES flux, but eruptive flares reveal on average a higher ribbon-separation velocity (by $\approx 10~$km$~$s$^{-1}$). The local reconnection electric field of confined ($cc=0.50~\pm~0.02$) and eruptive ($cc=0.77~\pm~0.03$) flares correlates with the GOES flux, indicating that more powerful flares involve stronger reconnection electric fields. In addition, eruptive flares with higher electric-field strengths tend to be accompanied by faster coronal mass ejections.