Comparison between IPSL Venus Global Climate Model results and aerobraking data

Abstract

<p align= justify ><span>For fifteen years</span><span>, a G</span><span>lobal</span><span> C</span><span>limate</span><span> Model (GCM) </span><span>ha</span><span>s </span><span>been</span><span> developed for the Venus atmosphere </span><span>at Institut Pierre-Simon Laplace (IPSL), in collaboration between LMD and LATMOS, </span><span>from the surface up to 150 km altitude. Its recent extension up to </span><span>the exobase (roughly </span><span>250 km</span><span>)</span><span> within the framework of the VCD project now allows us to simulate the Venusian upper atmosphere and the key atmospheric parameters of the aerobraking phases. The aim of this presentation is to study the evolution of the density of the Venusian upper atmosphere as a function of different parameters such as solar irradiance, </span><span>latitude, </span><span>local time and zenith solar angle (SZA), </span><span>for regions from 130 to 180 km of altitude.</span><span> We will present here several comparisons of the upper atmosphere of Venus between our model results and a selection of aerobraking data from different missions such as Venus Express, Pioneer Venus and Magellan. </span></p>