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Formation and evolution are key topics in planetary science, and we cannot fully understand planetary atmospheres without accounting for their interactions with the solar wind. The presence of aurora is an important manifestation and tracer of the interaction between the solar wind and planetary ionospheres. The OI (1S-1D) 557.7 nm (oxygen green line) is a bright auroral line in the terrestrial atmosphere and is detected on the Venusian nightside after major solar storms. Currently, the processes responsible for producing the green line emission on Venus are poorly understood, yet the observed variability of this feature is clearly linked to the solar wind environment. Here, we use the Wang – Sheeley – Arge (WSA) model and in situ data from Parker Solar Probe (PSP) to look at the solar wind conditions during a detection of the Venusian green line on 11 July 2020, when PSP was making its closest approach to Venus.