Scientific goals for the observation of Venus by VIRTIS on ESA/Venus express ffilSSlon
P. Drossarta,*, G. Piccionib, A. AdrianiC ; , F. Angrillid, G. Arnolde, K.H. Bainesf, G. Belluccib ; J. BenkhofF, B. Bezarda, J.-P. Bibrin, A. Blancoh, M.I. Bleckai, R.W. Carlsonf ; et al. ; - ASI Sponsor
Jan - 2007

journal : Planetaryand SpaceScience
type: Article Journal

Abstract
The Visible and Infrared ThermalImaging Spectrometer (VIRTIS) on board the ESAjVenus Express mission has technieal specifications well suited for many science objectives of Venus exploration. VIRTIS will both comprehensively explore a plethora of atmospheric properties and processes and map optical properties of the surface through its three channels, VIRTIS-M-vis (imaging spectrometer in the 0.3-1 J.1mrange), VIRTIS-M-IR (imaging spectrometer in the 1-5 J.1IDrange) and VIRTIS-H (aperture highresolution spectrometer in the 2-5 J.1mrange). The atmospheric composition below the clouds will be repeatedly measured in the night side infrared windows over a wide range of latitudes and longitudes, thereby providing information on Venuss chemieal cycles. In particular, CO, H20, OCS and S02 ean be studied. The cloud structure will be repeatedly mapped from the brightness contrasts in the near-infrared night sidewindows, providing new insights into Venusian meteorology. The global circulation and loeal dynamics ofVenus will beextensively studied from infrared and visible spectral images. The thermal structure above the clouds will be retrieved in the night side using the 4.3llm fundamental band of CO2• The surface of Venus is detectable in the short-wave infrared windows on the night side at 1.01, 1.10 and 1.18Ilm, providing constraints on surface properties and the extent ofactive volcanism. Many more tentative studies are also possible, such as lightning detection, the composition of volcanic emissions, and mesospheric wave propagation.

keywords : VENUS EXPRESS