Flare heating of the chromosphere: Observations of flare continuum from GREGOR and IRIS
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| Main Authors: | , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| author | García-Rivas, M. Kašparová, J. Berlicki, A. Švanda, M. Dudík, J. Čtvrtečka, D. Zapiór, M. Liu, W. Sobotka, M. Pavelková, M. Motorina, G. G. |
| author_facet | García-Rivas, M. Kašparová, J. Berlicki, A. Švanda, M. Dudík, J. Čtvrtečka, D. Zapiór, M. Liu, W. Sobotka, M. Pavelková, M. Motorina, G. G. |
| contents | Context: On 2022 May 4, an M5.7 flare erupted in the active region NOAA 13004, which was the target of a coordinated campaign between GREGOR, IRIS, Hinode, and ground-based instruments at the Ondřejov observatory. A flare kernel located at the edge of a pore was co-observed by the IRIS slit and GREGOR HiFI+ imagers. Aims: We investigated the flare continuum enhancement at different wavelength ranges in order to derive the temperature of the chromospheric layer heated during the flare. Methods: All datasets were aligned to IRIS slit-jaw images. We selected a pixel along the IRIS slit where the flare kernel was captured and evaluated multi-wavelength light curves within it. We defined a narrow IRIS near-UV band that comprises only continuum emission. The method, which assumes that the flare continuum enhancement is due to optically thin emission from hydrogen recombination processes, was applied to obtain a lower limit on the temperature in the layer where the continuum enhancement was formed. Results: We determined a lower limit for the temperature and its time evolution in the chromospheric layer heated during the flare in the range of (3-15).10^3 K. The mean electron density in that layer was estimated to be about 1.10^(13) cm^(-3). Conclusions: Multi-wavelength flare co-observations are a rich source of diagnostics. Due to the rapidly evolving nature of flares, the sit-and-stare mode is key to achieving a high temporal cadence that allows one to thoroughly analyse the same flare structure. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2408_10813 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Flare heating of the chromosphere: Observations of flare continuum from GREGOR and IRIS García-Rivas, M. Kašparová, J. Berlicki, A. Švanda, M. Dudík, J. Čtvrtečka, D. Zapiór, M. Liu, W. Sobotka, M. Pavelková, M. Motorina, G. G. Solar and Stellar Astrophysics Context: On 2022 May 4, an M5.7 flare erupted in the active region NOAA 13004, which was the target of a coordinated campaign between GREGOR, IRIS, Hinode, and ground-based instruments at the Ondřejov observatory. A flare kernel located at the edge of a pore was co-observed by the IRIS slit and GREGOR HiFI+ imagers. Aims: We investigated the flare continuum enhancement at different wavelength ranges in order to derive the temperature of the chromospheric layer heated during the flare. Methods: All datasets were aligned to IRIS slit-jaw images. We selected a pixel along the IRIS slit where the flare kernel was captured and evaluated multi-wavelength light curves within it. We defined a narrow IRIS near-UV band that comprises only continuum emission. The method, which assumes that the flare continuum enhancement is due to optically thin emission from hydrogen recombination processes, was applied to obtain a lower limit on the temperature in the layer where the continuum enhancement was formed. Results: We determined a lower limit for the temperature and its time evolution in the chromospheric layer heated during the flare in the range of (3-15).10^3 K. The mean electron density in that layer was estimated to be about 1.10^(13) cm^(-3). Conclusions: Multi-wavelength flare co-observations are a rich source of diagnostics. Due to the rapidly evolving nature of flares, the sit-and-stare mode is key to achieving a high temporal cadence that allows one to thoroughly analyse the same flare structure. |
| title | Flare heating of the chromosphere: Observations of flare continuum from GREGOR and IRIS |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2408.10813 |