Volatile in the martian crust as viewed from morphology of rampart crater

Details Volatile in the martian crust as viewed from morphology of rampart crater Volatile in the martian crust as viewed from morphology of rampart crater

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....5483k&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #5483

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Rampart crater is a unique and peculiar feature predominantly existing on Mars. This has been discussed as an evidence for existence of subsurface volatile in the martian crust. Recent progress in the morphological analysis based on the high resolution images by MGS has revealed the following important features; 1) Basic construct of the fresh rampart crater is the double lobate type composed of namely outer thin lobe and inner thick lobe. This means that a single impacting event generates at least two times of sedimentation events. 2) As for the sequence of these two emplacements, the inner thick lobe was formed first, then the outer thin lobe followed. 3) Dependence of the emplaced volume with the crater size is different between the inner lobe and the outer lobe. These lines of evidence indicate two lobes are formed by different mechanisms; ballistic emplacement for the inner lobe while emplacement by the surface gravity flow for the outer lobe. We present a summary of these based on data set for the rampart craters in the Casius region west of Elysium. Among the geomorphological features suggesting the nature of the outer lobe, radial scratch patterns remained on the surface of the inner lobe are particularly important. These scours, which are identified only on fresh craters, are considered to be caused by high velocity scratch by solid blocks contained in the outer lobe-forming flow. Because almost non of the massive blocks is identified along the extension of the scours in the high resolution images, these solid blocks should have disappeared since then. In this presentation we propose that solid blocks of CO2 hydrate clathrate exist among the materials forming the outer lobe. We discuss possibility of CO2 hydrate in the Martian crust as a solid reservoir of once-existed dense CO2 atmosphere.

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