# IRIS, Hinode, SDO, and RHESSI observations of a white light flare produced directly by non-thermal electrons

## TL;DR

This study combines multi-instrument observations to demonstrate that white light flare emission is directly caused by non-thermal electrons depositing energy in the solar atmosphere, supported by energy flux comparisons.

## Contribution

It provides direct observational evidence linking non-thermal electron energy flux to white light flare emission, enhancing understanding of flare energy transport mechanisms.

## Key findings

- White light emission correlates with hard X-ray peaks and evaporation flows.
- Energy flux from non-thermal electrons matches the energy needed for continuum enhancement.
- Explosive evaporation occurs concurrently with white light emission.

## Abstract

An X1.6 flare occurred in AR 12192 on 2014 October 22 at 14:02 UT and was observed by Hinode, IRIS, SDO, and RHESSI. We analyze a bright kernel which produces a white light (WL) flare with continuum enhancement and a hard X-ray (HXR) peak. Taking advantage of the spectroscopic observations of IRIS and Hinode/EIS, we measure the temporal variation of the plasma properties in the bright kernel in the chromosphere and corona. We found that explosive evaporation was observed when the WL emission occurred, even though the intensity enhancement in hotter lines is quite weak. The temporal correlation of the WL emission, HXR peak, and evaporation flows indicate that the WL emission was produced by accelerated electrons. To understand the white light emission process, we calculated the energy flux deposited by non- thermal electrons (observed by RHESSI) and compared it to the dissipated energy estimated from a chromospheric line (Mg II triplet) observed by IRIS. The deposited energy flux from the non-thermal electrons is about 3 ~ 7.7 X 10^(10) erg cm^(-2) s^(-1) for a given low energy cut-off of 30 ~ 40 keV, assuming the thick target model. The energy flux estimated from the temperature changes in the chromosphere measured using the Mg II subordinate line is about 4.6 - 6.7 X 10(9) erg cm^(-2) s^(-1): ~6-22% of the deposited energy. This comparison of estimated energy fluxes implies that the continuum enhancement was directly produced by the non-thermal electrons.