Ozone on Mars and Venus

Franck Montmessin 1 Jean-Loup Bertaux 1 Emmanuel Marcq 1
LATMOS - Laboratoire Atmosphères, Milieux, Observations Spatiales
Abstract : Cross-hemispheric circulation of the atmosphere is a major feature of the Martian troposphere and Venusian thermosphere. On Mars, it is driven by the latitudinal gradient of insolation at the surface, which generates a global summer-to-winter Hadley cell reversing orientation during equinoxes and maximizing intensity at solstices. On Venus, it is driven by a longitudinal gradient between the dayside and the nightside and takes place above the super-rotating mesosphere and troposphere. This subsolar-to-antisolar (SSAS) circulation is known to induce major observational features, such as the vast O2 and NO emission zones observed close to midnight. Recently, SPICAV onboard Venus Express has detected for the first time the presence of ozone on Venus, accounting for a thin thermospheric layer at about 100 km. Concomitantly, a similar feature was recently identified on Mars with SPICAM, with the presence of a >10 km thick ozone layer in the southern winter hemisphere near the pole.
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Soumis le : samedi 4 février 2012 - 14:30:42
Dernière modification le : jeudi 11 janvier 2018 - 02:06:26




Franck Montmessin, Jean-Loup Bertaux, Emmanuel Marcq. Ozone on Mars and Venus. EPSC-DPS Joint Meeting 2011, Oct 2011, Nantes, France. 〈hal-00666401〉



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