Abstract
Solar extreme ultraviolet (EUV) imaging instruments usually have a channel centered at 304 Å to observe the strong He ii 303.8 Å line, which is valuable for studying the dynamics of chromospheric and transition-region structures. In off-limb regions where He ii is weak, however, the coronal Si xi 303.3 Å line becomes significant and provides a background haze that reduces the contrast of He ii structures such as jets and macrospicules, complicating the interpretation of the observations. Generally, the separation of this background would require spectroscopic observations. In this article, we take an alternate approach by reconstructing the differential emission measure (DEM) of the quiescent corona to obtain synthetic radial emission profiles in the Si xi 303.3 Å line and show that at altitudes above 20 Mm it makes the major contribution to the background. We also find the silicon abundance to be significantly, by around 80%, lower in the quiet Sun than in the coronal hole. Based on the DEM profiles, we propose a physical model for the off-limb radial intensity profile in the Si xi 303.3 Å line. The model’s main advantage is the possibility to estimate and subtract the background of the quiescent corona using observations in the 304 Å channel alone, which may be of use for future studies of small-scale solar activity.
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Data Availability
All SDO/AIA data used in this work are courtesy of NASA/SDO and AIA science team and are available from the JSOC (jsoc.stanford.edu) without restriction.
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Acknowledgments
We gratefully acknowledge the use of data from the SDO/AIA, the CHIANTI database, and the DEM inversion code by Cheung et al. (2015). SDO is a mission for NASA’s Living With a Star (LWS) program. The data from the SDO/AIA are provided by the Joint Science Operations Center (JSOC) at Stanford University. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA), University of Cambridge (UK), and NASA Goddard Space Flight Center (USA). We also thank the anonymous reviewer for carefully reading the manuscript and for useful suggestions, which helped to significantly improve our work and the clarity of its presentation.
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This research was funded by a grant from the Russian Science Foundation (grant No 21-72-10157, rscf.ru/project/21-72-10157).
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I. Loboda and A. Reva wrote the main manuscript text. A. Kirichenko obtained the observational data and performed its initial processing. I. Loboda and A. Ulyanov performed DEM reconstruction and obtained synthetic intensity profiles. A. Reva and S. Bogachev prepared the figures for the manuscript. All authors have reviewed the manuscript.
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Loboda, I., Reva, A., Bogachev, S. et al. Separating He ii and Si xi Emission Components in Off-limb 304 Å Observations. Sol Phys 298, 136 (2023). https://doi.org/10.1007/s11207-023-02230-6
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DOI: https://doi.org/10.1007/s11207-023-02230-6