Probing progression of heating through the lower flare atmosphere via high-cadence IRIS spectroscopy
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arXiv
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| Format: | Preprint |
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2025
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| author | Lörinčík, Juraj Polito, Vanessa Kerr, Graham S. Hayes, Laura A. Russell, Alexander J. B. |
| author_facet | Lörinčík, Juraj Polito, Vanessa Kerr, Graham S. Hayes, Laura A. Russell, Alexander J. B. |
| contents | Recent high-cadence flare campaigns by the Interface Region Imaging Spectrograph (IRIS) have offered new opportunities to study rapid processes characteristic of flare energy release, transport, and deposition. Here, we examine high-cadence chromospheric and transition region spectra acquired by IRIS during a C-class flare from 2022 September 25. Within the flare ribbon, the intensities of the Si IV 1402.77, C II 1334.53 and Mg II k 2796.35 lines peaked at different times, with the transition region Si IV typically peaking before the chromospheric Mg II line by 1 - 6 seconds. To understand the nature of these delays, we probed a grid of radiative hydrodynamic flare simulations heated by electron beams, thermal conduction-only, or Alfvén waves. Electron beam parameters were constrained by hard X-ray observations from the Gamma-ray Burst Monitor (GBM) onboard the Fermi spacecraft. Reproducing lightcurves where Si IV peaks precede those in Mg II proved to be a challenge, as only a subset of Fermi/GBM-constrained electron beam models were consistent with the observations. Lightcurves with relative timings consistent with the observations were found in simulations heated by either high-flux electron beams or by Alfvén waves, while the thermal conduction heating does not replicate the observed delays. Our analysis shows how delays between chromospheric and transition region emission pose tight constraints on flare models and properties of energy transport, highlighting the importance of obtaining very high-cadence datasets with IRIS and other observatories. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_10619 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Probing progression of heating through the lower flare atmosphere via high-cadence IRIS spectroscopy Lörinčík, Juraj Polito, Vanessa Kerr, Graham S. Hayes, Laura A. Russell, Alexander J. B. Solar and Stellar Astrophysics Recent high-cadence flare campaigns by the Interface Region Imaging Spectrograph (IRIS) have offered new opportunities to study rapid processes characteristic of flare energy release, transport, and deposition. Here, we examine high-cadence chromospheric and transition region spectra acquired by IRIS during a C-class flare from 2022 September 25. Within the flare ribbon, the intensities of the Si IV 1402.77, C II 1334.53 and Mg II k 2796.35 lines peaked at different times, with the transition region Si IV typically peaking before the chromospheric Mg II line by 1 - 6 seconds. To understand the nature of these delays, we probed a grid of radiative hydrodynamic flare simulations heated by electron beams, thermal conduction-only, or Alfvén waves. Electron beam parameters were constrained by hard X-ray observations from the Gamma-ray Burst Monitor (GBM) onboard the Fermi spacecraft. Reproducing lightcurves where Si IV peaks precede those in Mg II proved to be a challenge, as only a subset of Fermi/GBM-constrained electron beam models were consistent with the observations. Lightcurves with relative timings consistent with the observations were found in simulations heated by either high-flux electron beams or by Alfvén waves, while the thermal conduction heating does not replicate the observed delays. Our analysis shows how delays between chromospheric and transition region emission pose tight constraints on flare models and properties of energy transport, highlighting the importance of obtaining very high-cadence datasets with IRIS and other observatories. |
| title | Probing progression of heating through the lower flare atmosphere via high-cadence IRIS spectroscopy |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2504.10619 |