Observational Evidences of Electron-driven Evaporation in two Solar Flares

TL;DR

This study provides observational evidence linking electron-driven chromospheric evaporation to hard X-ray emissions during two significant solar flares, highlighting the dynamic relationship between plasma motions and energetic particles.

Contribution

It presents direct spectroscopic observations of chromospheric evaporation correlated with HXR emissions, confirming electron-driven processes in two large solar flares.

Findings

Fe XXI shows blue shifts during impulsive phase

C I shows red shifts during impulsive phase

Doppler velocities correlate with HXR emission phases

Abstract

We have explored the relationship between hard X-ray (HXR) emissions and Doppler velocities caused by the chromospheric evaporation in two X1.6 class solar flares on 2014 September 10 and October 22, respectively. Both events display double ribbons and Interface Region Imaging Spectrograph (IRIS) slit is fixed on one of their ribbons from the flare onset. The explosive evaporations are detected in these two flares. The coronal line of Fe XXI 1354.09 A shows blue shifts, but chromospheric line of C I 1354.29 A shows red shifts during the impulsive phase. The chromospheric evaporation tends to appear at the front of flare ribbon. Both Fe XXI and C I display their Doppler velocities with a `increase-peak-decrease' pattern which is well related to the `rising-maximum- decay' phase of HXR emissions. Such anti-correlation between HXR emissions and Fe XXI Doppler shifts, and correlation with C I Doppler shifts indicate the electron-driven evaporation in these two flares.