Structure of the Venus atmosphere

By L. Zasova, N. Ignatiev, I. Khatuntsev, V. Linkin. 2007

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Clouds and Hazes of Venus (2018, methodology): “The data analysis included retrievals of the temperature structure, calculation of the thermal winds in the mesosphere, determination of H2O and SO2 abundance at the cloud top, and assessment of the upper cloud parameters (see Zasova et al. 2007 and references therein).”
Superrotation of Venus' atmosphere analyzed with a full general circulation model (2010, methodology): “This is much lower than variations seen in available observations, that may reach 20–30 K at 50 km altitude [Seiff et al., 1980; Sromovsky et al., 1985; Zasova et al., 2007; Tellmann et al., 2009].”
The Atmospheric Dynamics of Venus (2017, methodology): “…occultation measurements from Pioneer Venus, the Venera-15 and Venus Express orbiters (Seiff et al. 1980, Taylor et al. 1980; Lellouch et al. 1997; Zasova et al. 2007; Tellmann et al. 2009) have been used in various attempts to reconstruct Venus’ zonal winds (Limaye 1985; Roos-Serote et al. 1995;…”