The spatial distribution of volatiles in the Martian hydrolithosphere

  title={The spatial distribution of volatiles in the Martian hydrolithosphere},
  author={François Costard},
  journal={Earth, Moon, and Planets},
  • F. Costard
  • Published 1 June 1989
  • Geology
  • Earth, Moon, and Planets
In order to quantify the spatial distribution of volatiles on Mars, 2600 fluidized ejecta craters have been systematically measured, classified and mapped over the planet Mars, using 1 : 2 M scale USGS photomosaics. The latitudinal distribution of ejecta craters reveals that flower ejecta deposits (Type 1), together with low mobility ejecta, are frequently observed in the equatorial region and on ridged plains. Rampart craters (Type 2), with high mobility ejecta, occur at mid latitudes and… 
Insights into complex layered ejecta emplacement and subsurface stratigraphy in Chryse Planitia, Mars, through an analysis of THEMIS brightness temperature data
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Martian perched craters and large ejecta volume: Evidence for episodes of deflation in the northern lowlands
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The origin and timing of fluvial activity at Eberswalde crater, Mars
Volatile history of Mangala Valles, Mars
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Evidence of ancient continental glaciation in the Martian northern plains
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Observations of Martian layered ejecta craters and constraints on their formation mechanisms
The formation mechanism of layered ejecta craters on Mars has remained a topic of intense debate since their discovery. In this study, we perform a global morphological analysis of Martian layered


Effects of elevation and ridged plains thicknesses on Martian crater ejecta morphology
Relationships between the distribution of Martian crater ejecta morphologies and both elevation and ridged plains thicknesses have been investigated. We observed a slight correlation between
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Kilometer to subkilometer cones with large central craters are the most numerous volcanic structures in the northern plains of Mars. Based on examination of more than 12,000 high resolution Viking
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The lowland plains on Mars have surfaces marked by large polygonal fracture patterns. It was recently proposed that the fracture patterns were developed on sedimentary deposits from outflow channels.
Martian impact craters and emplacement of ejecta by surface flow
Several types of Martian impact craters have been recognized. The most common type, the rampart crater, is distinctively different from lunar and Mercurian craters. It is typically surrounded by
The distribution of lobate debris aprons and similar flows on Mars
Planet-wide mapping of lobate debris aprons and other similar flows on Mars shows a strong concentration in two latitudinal bands roughly 25° wide and centered at 40°N and 45°S. This distribution