Infrared spectropolarimetry of a C-class solar flare footpoint plasma -- I. Spectral features and forward modelling
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| Natura: | Preprint |
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2026
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| author | Vashalomidze, Z. Noda, C. Quintero Zaqarashvili, T. V. Benko, M. Kuridze, D. Gömöry, P. Rybák, J. Lomineishvili, S. Collados, M. Denker, C. Verma, M. Kuckein, C. Ramos, A. Asensio |
| author_facet | Vashalomidze, Z. Noda, C. Quintero Zaqarashvili, T. V. Benko, M. Kuridze, D. Gömöry, P. Rybák, J. Lomineishvili, S. Collados, M. Denker, C. Verma, M. Kuckein, C. Ramos, A. Asensio |
| contents | 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 Å, Ca I 10833.4 Å, Na I 10834.9 Å, and Ca I 10838.9 Å photospheric lines, as well as the He I 10830 Å 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 Å triplet signals in the future. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2602_20798 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Infrared spectropolarimetry of a C-class solar flare footpoint plasma -- I. Spectral features and forward modelling Vashalomidze, Z. Noda, C. Quintero Zaqarashvili, T. V. Benko, M. Kuridze, D. Gömöry, P. Rybák, J. Lomineishvili, S. Collados, M. Denker, C. Verma, M. Kuckein, C. Ramos, A. Asensio Solar and Stellar Astrophysics 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 Å, Ca I 10833.4 Å, Na I 10834.9 Å, and Ca I 10838.9 Å photospheric lines, as well as the He I 10830 Å 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 Å triplet signals in the future. |
| title | Infrared spectropolarimetry of a C-class solar flare footpoint plasma -- I. Spectral features and forward modelling |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2602.20798 |