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Open AccessArticle

Validation of the IPSL Venus GCM Thermal Structure with Venus Express Data

1
INAF-IAPS, Istituto di Astrofisica e Planetologia Spaziali, 00133 Rome, Italy
2
Department of Physics, University of Rome Tor Vergata, 00133 Rome, Italy
3
Escuela de Ingeniería de Bilbao, Universidad del País Vasco / Euskal Herriko Unibertsitatea, 48013 Bilbao, Spain
4
Laboratoire de Météorologie Dynamique (LMD/IPSL), Sorbonne Université, ENS, PSL Research University, Ecole Polytechnique, Institute Polytechnique de Paris, CNRS, 75252 Paris, France
5
Department of Planetary Research, Rheinisches Institut fr Umweltforschung at the University of Cologne, Aachener Str. 209, 50931 Cologne, Germany
*
Author to whom correspondence should be addressed.
Atmosphere 2019, 10(10), 584; https://doi.org/10.3390/atmos10100584
Received: 16 August 2019 / Revised: 21 September 2019 / Accepted: 24 September 2019 / Published: 26 September 2019
(This article belongs to the Special Issue Modeling and Simulation of Planetary Atmospheres)
General circulation models (GCMs) are valuable instruments to understand the most peculiar features in the atmospheres of planets and the mechanisms behind their dynamics. Venus makes no exception and it has been extensively studied thanks to GCMs. Here we validate the current version of the Institut Pierre Simon Laplace (IPSL) Venus GCM, by means of a comparison between the modelled temperature field and that obtained from data by the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) and the Venus Express Radio Science Experiment (VeRa) onboard Venus Express. The modelled thermal structure displays an overall good agreement with data, and the cold collar is successfully reproduced at latitudes higher than +/−55°, with an extent and a behavior close to the observed ones. Thermal tides developing in the model appear to be consistent in phase and amplitude with data: diurnal tide dominates at altitudes above 102 Pa pressure level and at high-latitudes, while semidiurnal tide dominates between 102 and 104 Pa, from low to mid-latitudes. The main difference revealed by our analysis is located poleward of 50°, where the model is affected by a second temperature inversion arising at 103 Pa. This second inversion, possibly related to the adopted aerosols distribution, is not observed in data. View Full-Text
Keywords: Venus atmosphere; thermal structure; thermal tides; data-model comparison; modelling Venus atmosphere; thermal structure; thermal tides; data-model comparison; modelling
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Scarica, P.; Garate-Lopez, I.; Lebonnois, S.; Piccioni, G.; Grassi, D.; Migliorini, A.; Tellmann, S. Validation of the IPSL Venus GCM Thermal Structure with Venus Express Data. Atmosphere 2019, 10, 584.

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