HR: 17:20h
AN: P34A-05    [Abstracts]
TI: Martian Gullies: H2O or CO2 snow?
AU: * Yolanda, C
EM: yolanda@soho.igeofcu.unam.mx
AU: Durand-Manterola, H J
EM: hdurand_manterola@yahoo.com
AB: The theories proposed to try to explain the origin of the Martian gullies involve either liquid water, liquid carbon dioxide or flows of dry granular material. We propose another processes that can be favorable for the origin of the Martian gullies, with our model by gaseous fluidification of CO2. We propose that on the Martian slopes, CO2 snow and dust transported by winds, are accumulate. During the Martian spring, sublimation of carbonic snow starts because of heat and weigth of the frezze layer, causing that the material mixed its fluidifized and slide downslope by gravity. By experimental work with dry granular material, we simulated the development of the Martian gullies injecting air inside the granular material. We also present the characteristics of some terrestrial gullies forms at cold environment, sited at Nevado de Toluca Volcano near Toluca City, México. We compared them with some Martian gullies, to identify possible processes evolved in its formation. We measured the lengths of those Martian gullies and the range was from 24 meters to 1775 meters. Finally, we present results of our experimental work at laboratory with dry granular material and our field trip to Nevado de Toluca Volcano.
DE: 5415 Erosion and weathering
SC: Planetary Sciences [P]
MN: 2007 Joint Assembly