Exploring mutual information between IRIS spectral lines. II. Calculating the most probable response in all spectral windows

TL;DR

This paper extends previous work on solar spectral line correlations to determine the most probable atmospheric responses during flares, using IRIS spectral data to analyze multi-line behavior and correlations across different solar regions.

Contribution

It introduces a framework for predicting spectral responses across multiple lines from single spectra, based on extensive IRIS data, enhancing understanding of solar flare atmospheric dynamics.

Findings

Strong correlations in flare ribbons across spectral lines

Simultaneous blue-shifts in Mg II, C II, Si IV during impulsive phase

Evolution of Mg II line profiles from blue-shifted to single peaked

Abstract

A three-dimensional picture of the solar atmosphere's thermodynamics can be obtained by jointly analyzing multiple spectral lines that span many formation heights. In paper I, we found strong correlations between spectral shapes from a variety of different ions during solar flares in comparison to the quiet Sun. We extend these techniques to address the following questions: which regions of the solar atmosphere are most connected during a solar flare, and what are the most likely responses across several spectral windows based on the observation of a single Mg II spectrum? Our models are derived from several million IRIS spectra collected from 21 M- and X-class flares. We applied this framework to archetypal Mg II flare spectra, and analyzed the results from a multi-line perspective. We find that (1) the line correlations from the photosphere to the transition region are highest in flare ribbons. (2) Blue-shifted reversals appear simultaneously in Mg II, C II, and Si IV during the impulsive phase, with Si IV displaying possible optical depth effects. Fe II shows signs of strong emission, indicating deep early heating. (3) The Mg II line appears to typically evolve a blue-shifted reversal that later returns to line center and becomes single peaked within 1-3 minutes. The widths of these single peaked profiles slowly erode with time. During the later flare stages, strong red wing enhancements indicating coronal rain are evident in Mg II, C II, and Si IV. Our framework is easily adaptable to any multi-line data set, and enables comprehensive statistical analyses of the atmospheric behavior in different spectral windows.