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. 2020 Feb 26;10:3448. doi: 10.1038/s41598-020-59278-8

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© The Author(s) 2020

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 license, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons license, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons license 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 license, visit http://creativecommons.org/licenses/by/4.0/.

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Comparison of the mean static stability obtained from radio occultation measurements (black) with VIRA (red), VIRA-2 (blue) and Magellan radio occultation measurements (green). In each panel, the number within parentheses is the number of radio occultation measurements made at an altitude of 50 km. Latitudinal ranges are (a) 0°–30°, (b) 30°–60°, (c) 60°–70°, (d) 70°–80° and (e) 80°–90°, and the altitude range is 40–85 km. Only at latitudes of 0°–30°, the radio occultation data are divided into those obtained on Venus Express (black) and Akatsuki (green) missions. Static stability obtained from radio occultation measurements are zonally and temporally averaged. Error bars in each panel represent the standard deviation of the static stability obtained from radio occultation measurements.