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| Natura: | Preprint |
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2026
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| Accesso online: | https://arxiv.org/abs/2601.17491 |
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| _version_ | 1866911396707434496 |
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| author | Phillips, Kenneth J. H. Sylwester, Barbara Sylwester, Janusz |
| author_facet | Phillips, Kenneth J. H. Sylwester, Barbara Sylwester, Janusz |
| contents | Archived high-resolution X-ray spectra in the 13~Å to 22~Å range from the Flat Crystal Spectrometer (FCS), an instrument on the Solar Maximum Mission operating in the 1980s, are analyzed with reference to nonflaring active regions, and to the \ion{Fe}{17} line emission in light of laboratory and atomic data for nearby \ion{Fe}{16} satellites. The satellites allow temperature to be found for these relatively low-temperature spectra, at which more conventional temperature-dependent line ratios are unavailable. By this means, the spectra can be arranged by temperature, showing that the \ion{Fe}{17} lines are evident at temperatures of $<3$~MK. We confirm that the problem of the underintense Fe XVII 3C and 3D lines is not due to resonant scattering, and instead suggest that, for comparison with CHIANTI spectra, the problem may lie with a needed revision of collisional excitation rates. The line ratio 3G/3H is in theory density-dependent but for \ion{Fe}{17} the ratio is in the low-density limit. However, we suggest that spectra taken during the impulsive stage of flares might reveal a departure from this limit and so allow densities to be derived and hence properties of the flaring plasma. Suggestions for the design of future crystal spectrometers are made in the light of the fluorescence background in FCS spectra. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2601_17491 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | High-Resolution Solar X-ray Spectroscopy from Archived Solar Maximum Mission Data Phillips, Kenneth J. H. Sylwester, Barbara Sylwester, Janusz Solar and Stellar Astrophysics Archived high-resolution X-ray spectra in the 13~Å to 22~Å range from the Flat Crystal Spectrometer (FCS), an instrument on the Solar Maximum Mission operating in the 1980s, are analyzed with reference to nonflaring active regions, and to the \ion{Fe}{17} line emission in light of laboratory and atomic data for nearby \ion{Fe}{16} satellites. The satellites allow temperature to be found for these relatively low-temperature spectra, at which more conventional temperature-dependent line ratios are unavailable. By this means, the spectra can be arranged by temperature, showing that the \ion{Fe}{17} lines are evident at temperatures of $<3$~MK. We confirm that the problem of the underintense Fe XVII 3C and 3D lines is not due to resonant scattering, and instead suggest that, for comparison with CHIANTI spectra, the problem may lie with a needed revision of collisional excitation rates. The line ratio 3G/3H is in theory density-dependent but for \ion{Fe}{17} the ratio is in the low-density limit. However, we suggest that spectra taken during the impulsive stage of flares might reveal a departure from this limit and so allow densities to be derived and hence properties of the flaring plasma. Suggestions for the design of future crystal spectrometers are made in the light of the fluorescence background in FCS spectra. |
| title | High-Resolution Solar X-ray Spectroscopy from Archived Solar Maximum Mission Data |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2601.17491 |