quarta-feira, 16 de abril de 2014
Low palaeopressure of the martian atmosphere estimated from the size distribution of ancient craters
The decay of the martian atmosphere—which is dominated by carbon dioxide—is a component of the long-term environmental change on Mars1 from a climate that once allowed rivers to flow2, 3, 4, 5, 6 to the cold and dry conditions of today. The minimum size of craters serves as a proxy for palaeopressure of planetary atmospheres, because thinner atmospheres permit smaller objects to reach the surface at high velocities and form craters7, 8, 9. The Aeolis Dorsa region near Gale crater on Mars contains a high density of preserved ancient craters interbedded with river deposits11 and thus can provide constraints on atmospheric density at the time of fluvial activity. Here we use high-resolution images and digital terrain models10 from the Mars Reconnaissance Orbiter to identify ancient craters in deposits in Aeolis Dorsa that date to about 3.6 Gyr ago and compare their size distribution with models of atmospheric filtering of impactors12, 13. We obtain an upper limit of 0.9 ± 0.1 bar for the martian atmospheric palaeopressure, rising to 1.9 ± 0.2 bar if rimmed circular mesas—interpreted to be erosionally-resistant fills or floors of impact craters—are excluded. We assume target properties appropriate for desert alluvium14: if sediment had rock-mass strength similar to bedrock at the time of impact, the paleopressure upper limit increases by a factor of up to two. If Mars did not have a stable multibar atmosphere at the time that the rivers were flowing—as suggested by our results—then a warm and wet CO2/H2O greenhouse2 is ruled out, and long-term average temperatures were most likely below freezing.
Nature Geoscience (2014) doi:10.1038/ngeo2137 Published online 13 April 2014