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Catalogue POP – Notice individuelle de publication

Drossart Pierre, Piccioni Giuseppe, Adriani Alberto, Angrilli Francesco, Arnold Gabriele, Baines Kevin H., Bellucci Giancarlo, Benkhoff Johann, Bézard Bruno, Bibring Jean-Pierre, Blanco A., Blecka M. I., Carlson Robert W., Coradini Angioletta, Di Lellis A., Encrenaz Thérèse, Erard Stéphane, Fonti Sergio, Formisano Vittorio, Fouchet Thierry, Garcia R., Haus Rainer, Helbert Jörn, Ignatiev Nikolay I., Irwin Patrick G. J., Langevin Yves, Lebonnois Sebastien, Lopez-Valverde Miguel, Luz David, Marinangeli Lucia, Orofino Vincenzo, Rodin Alexander, Roos-Serote Maarten, Saggin B., Sánchez-Lavega Agustín, Stam Daphne, Taylor Frederic W., Titov Dmitry V., Visconti G., Zambelli M., Hueso R., Tsang Constantine C. C., Wilson Colin F., Afanasenko T. Z.

Scientific goals for the observation of Venus by VIRTIS on ESA/Venus express mission

Planetary and Space Science, 2007, vol. 55, pp. 1653-1672

Référence DOI : 10.1016/j.pss.2007.01.003
Référence ADS : 2007P&SS...55.1653D

Résumé :

The Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) on board the ESA/Venus Express mission has technical 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 mum range), VIRTIS-M-IR (imaging spectrometer in the 1-5 mum range) and VIRTIS-H (aperture high-resolution spectrometer in the 2-5 mum range). 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 Venus's chemical cycles. In particular, CO, H <SUB>2</SUB>O, OCS and SO <SUB>2</SUB> can be studied. The cloud structure will be repeatedly mapped from the brightness contrasts in the near-infrared night side windows, providing new insights into Venusian meteorology. The global circulation and local dynamics of Venus will be extensively studied from infrared and visible spectral images. The thermal structure above the clouds will be retrieved in the night side using the 4.3 mum fundamental band of CO <SUB>2</SUB>. The surface of Venus is detectable in the short-wave infrared windows on the night side at 1.01, 1.10 and 1.18 mum, providing constraints on surface properties and the extent of active volcanism. Many more tentative studies are also possible, such as lightning detection, the composition of volcanic emissions, and mesospheric wave propagation.

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