{"id":4543,"date":"2025-04-29T17:09:13","date_gmt":"2025-04-29T15:09:13","guid":{"rendered":"https:\/\/academiespatiale.fr\/?post_type=tribe_events&p=4543"},"modified":"2025-04-29T17:09:30","modified_gmt":"2025-04-29T15:09:30","slug":"seminaire-latmos-suivre-les-tempetes-de-poussiere-martiennes","status":"publish","type":"tribe_events","link":"https:\/\/academiespatiale.fr\/index.php\/event\/seminaire-latmos-suivre-les-tempetes-de-poussiere-martiennes\/","title":{"rendered":"[S\u00e9minaire – LATMOS] Suivre les temp\u00eates de poussi\u00e8re martiennes"},"content":{"rendered":"
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\n\t\t\n\t\t\t13 mai 2025\t\t<\/span>\n\n\t\t\t\t\t\n\t\t\t\t : \t\t\t<\/span>\n\t\t\t\n\t\t\t\t11h30\t\t\t<\/span>\n\t\t\n\t\t\t\t\t\t\t\t\t\n\t\t\t\t\t–\t\t\t\t<\/span>\n\t\t\t\n\t\t\t\t\t\t\t\n\t\t\t\t\t13h00\t\t\t\t<\/span>\n\t\t\t\n\t\t\t\t\t\t<\/p>\n<\/div>\n\n\n\n

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Yann Leseigneur, Enseignant-chercheur au LATMOS, donnera un s\u00e9minaire sur \u00ab Suivre les temp\u00eates de poussi\u00e8re martiennes \u00e0 travers les \u00e9chelles et les instruments \u00bb. Le s\u00e9minaire aura lieu \u00e0 11h30 au LATMOS \u00e0 Guyancourt en salle 2202 et sera retransmis sur Zoom.<\/p>\n\n\n\n

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Suivre les temp\u00eates de poussi\u00e8re martiennes \u00e0 travers les \u00e9chelles et les instruments.<\/strong><\/p>\n\n\n\n

Mardi 13 mai 2025<\/strong>
11h30
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LATMOS
Salle 2202
11, boulevard d’Alembert
Guyancourt<\/p>\n\n\n\n

En visioconf\u00e9rence<\/strong>
https:\/\/cnrs.zoom.us\/j\/93475642647?pwd=TQozK3ojmp6o26BrEDCXASjVduhERP.1<\/a>
ID de r\u00e9union: 934 7564 2647
Code secret: ndpAc7<\/p>\n\n\n\n

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Abstract:<\/p>\n\n\n\n

The Martian dust, composed of micrometer-size mineral particles, plays a key role on Mars, modifying, for example, the atmosphere\u2019s circulation, the surface heat balance, and is also involved in the atmospheric escape. On Mars, there is a dust cycle composed of: dust lifting from the surface and injection into the atmosphere by mechanisms that are not well understood (e.g., wind, saltations); dust movements and formation of dust storms that cover large scales (from sub-km to planetary scale, and from the minute to months); sedimentation that redistribute dust on the surface on a regional and global scale. Note that this cycle is connected to some surface movements, such as the Recurring Slope Lineae (RSL), which are seasonal dark movements forming on steep slopes. The Martian dust has been observed for decades from orbit, mostly using global imagers (UV & VIS) and thermal IR spectrometers. The limitations of these instruments are: very limited coverage of dust phenomena at small\/local scale (< 2000 km), and quantification of atmospheric dust at a few thermal wavelengths. Therefore, questions remain, for example, on the activity of the local dust storms, on the formation and growth mechanisms of dust storms, on the dust diurnal variations, on the link between all the length scales, or on the planetary dust storm formations.
I will present the different dust detection methods using archive data, notably a technique applied to OMEGA\/Mars Express (near-IR spectrometer), which allows studying dust storms at local scale and complements other studies at regional scale. We will also talk about the preparation of future observations of MIRS\/MMX (near-IR spectrometer), which will allow studying, for example, the diurnal variations of the atmospheric dust and hopefully allow catching the formation and growth of a dust storm at high temporal and spatial resolution.<\/p>\n\n\n\n

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