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. 2023 Jun 14;298(6):78. doi: 10.1007/s11207-023-02170-1

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© The Author(s) 2023

Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/.

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The proportion of the total emissivity contributed by resonant scattering as a function of height, for various fractions [ $B$ ] of the model value of the solar-wind speed, as reported in Gilly and Cranmer (2020). $B$ is a scalar factor applied to the radial-wind-speed profile, with $B = 0$ indicating no wind and $B = 1$ indicating wind at nominal modeled values. Ion-line wavelengths are given in units of angstroms. (Figure 17 of Gilly and Cranmer, 2020, used with permission).