Infrared spectropolarimetry of a C-class solar flare footpoint plasma -- I. Spectral features and forward modelling

TL;DR

This study uses high-resolution infrared spectropolarimetry to analyze the spectral features and plasma dynamics during a C-class solar flare, revealing complex chromospheric responses and flare-related flows.

Contribution

It provides detailed spectral analysis and forward modelling of flare-related spectral features, highlighting the complex chromospheric response and plasma flows during a C-class solar flare.

Findings

Detection of Doppler velocities up to 90 km/s in spectral lines.

Flare did not alter the physical conditions of the lower photosphere.

He I line emission reflects a complex chromospheric response.

Abstract

We performed high-spatial resolution spectropolarimetric observations of active region NOAA 13363 during a C-class flare with the Gregor Infrared Spectrograph (GRIS) on 16 July 2023. We examine the coupling between the photosphere and the chromosphere, studying the polarimetric signals during a period that encompasses the decaying phase of a C-class flare and the appearance of a new C-class flare at the same location. We focus on the analysis of various spectral lines. In particular, we study the Si I 10827 {\AA}, Ca I 10833.4 {\AA}, Na I 10834.9 {\AA}, and Ca I 10838.9 {\AA} photospheric lines, as well as the He I 10830 {\AA} triplet. GRIS data revealed the presence of flare-related red- and blueshifted spectral line components, reaching Doppler velocities up to 90 km/s, and complex Si I profiles where the He i spectral line contribution is blueshifted. In contrast, the photospheric Ca i and Na i transitions remained unchanged, indicating that the flare did not modify the physical conditions of the lower photosphere. We combined that information with simultaneous imaging in the Ca ii H line and TiO band with the improved High-resolution Fast Imager (HiFI+), finding that the flare emission did not affect the inverse granulation or nearby plage, in agreement with the results from GRIS. We also complement the previous studies with a forward modelling computation, concluding that the He I spectral line emission reflects a complex response of the flaring chromosphere. Radiative excitation from coronal EUV irradiation, energy deposition by flare-accelerated electrons, and dynamic field-aligned plasma flows likely act together to produce the observed supersonic downflows and upflows. We plan to expand these findings through inversions of the He I 10830 {\AA} triplet signals in the future.