profiles closely resemble the observational data, including a continuum enhancement, and both a stationary and a highly red-shifted component, rapidly moving towards the rest wavelength. Importantly, the absolute continuum intensity, ratio of component intensities, relative time of appearance, and red-shift amplitude, are sensitive to the model input parameters, showing great potential as diagnostics.
author:
- 'David R. Graham'
- Gianna Cauzzi
- Luca Zangrilli
- Adam Kowalski
- Paulo Simões
- Joel Allred
bibliography:
- 'flarebibliogc.bib'
title: Spectral signatures of chromospheric condensation in a major solar flare
---

Introduction {#sec:intro}
============

Solar flares bear on multiple aspects of plasma physics, including the physics of magnetic reconnection, the transport of energy from the corona to the lower atmosphere, the production of coronal mass ejections driving space weather, etc. [@2011LRSP....8....6S; @2017LRSP...14....2B]. The solar flare paradigm remains widely accepted as a template for magnetic activity on other stars [e.g. @2017ApJ...851...91N], thus a full understanding of the phenomenon has a large relevance for astrophysics in general.

In particular, the chromosphere remains a crucial element to understand the development of flares. While the primary energy release mechanism is governed by magnetic reconnection in the corona, the chromosphere is the location where this energy is ultimately 