Spectroscopic analysis and RHD modeling of the first Ca II H and H-epsilon flare spectra from DKIST/ViSP

TL;DR

This study presents high-resolution DKIST spectroscopic observations of a solar flare's decay phase, focusing on Ca II H and H-epsilon lines, and compares them with advanced radiative hydrodynamic models to evaluate their accuracy.

Contribution

It provides the first detailed comparison of DKIST flare spectra with RADYN+RH simulations, highlighting model limitations and suggesting improvements for understanding flare heating mechanisms.

Findings

Models reproduce some spectral properties like H-epsilon width.

Models underestimate Ca II H red wing width and relative intensity.

H-epsilon width is influenced by deeper flare layers, not just condensation properties.

Abstract

We analyze decay phase observations of the GOES class C6.7 flare SOL2022-08-19T20:31 by the Visible Spectropolarimeter (ViSP) on the National Science Foundation's Daniel K. Inouye Solar Telescope (DKIST). The data include the first flare-time DKIST observations of the chromospheric Ca II H 396.8 nm and H-epsilon 397.0 nm spectral lines. These diagnostics have rarely been studied together during the modern era of high-resolution solar flare observations, and never at the spectral and spatial resolution of the DKIST. We directly compare DKIST spectra to state-of-the-art RADYN+RH simulations, including one heated by a nonthermal electron beam and one by in-situ thermal conduction. While certain salient properties of the spectra such as the width of H-epsilon are reproduced, the models severely underestimate the width of Ca II H in the red wing and fail to reproduce the exact relative intensity of Ca II H to H-epsilon. The models exhibit a range of condensation electron densities spanning over an order of magnitude. Unlike the modeled lower-order Balmer-series lines, we find that the width of H-epsilon is not solely related to the condensation properties; the widths and intensities are also sensitive to the deeper flare layers. We outline possible avenues towards improvement of flare models, such as a comprehensive evaluation of flare heating mechanisms in the context of both impulsive and decay phase high-resolution data.