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• W1553006072 abstract "Introduction: Martian impact craters display a range of morphologic and morphometric variations. Previous analyses of central pit, central peak, and elliptical craters on Mars were conducted using the Catalog of Large Martian Impact Craters (Catalog 1.0), compiled from Viking data [1-3]. Catalog 1.0 is being revised (Catalog 2.0) using Mars Global Surveyor (MGS) and Mars Odyssey data [4]. Updating of northern hemisphere craters is complete, allowing comparisons between the two Catalog versions in this region. Here we report on results for central pit, central peak, and elliptical craters in Mars’ northern hemisphere. Catalog Comparison: Catalog 1.0 contained information on 12,920 craters ≥5-km-diameter in the northern hemisphere. Improved image resolutions and clarity provided by Odyssey’s Thermal Emission Imagining System (THEMIS) instrument has resulted in identification of 14,225 craters ≥5-km-diameter, an ~10% increase. All craters in Catalog 1.0 were reviewed: diameters were remeasured using ArcGIS tools, coordinates updated to MDIM 2.1 [5], and ejecta and interior classifications revised based on THEMIS image analysis [6]. Catalog 1.0 craters were generally have diameters within 10% of their Catalog 2.0 values. Preservation state of Catalog 2.0 craters was classified on a 0.0-7.0 scale, with 0.0 corresponding to a “ghost” crater and 7.0 being a pristine crater [7]. Although preservation state is a proxy for crater age, the variety of geologic processes operating across Mars throughout its history means that craters of similar preservation state in widely separated regions of the planet may not be contemporaneous. Central Pit Craters: Martian impact craters, like those on Ganymede and Callisto, often display central pits [8], which can occur either directly on the crater floor (“floor pits”) or atop a central rise or peak (“summit pits”). The number of craters classified as floor pits has increased from 165 in Catalog 1.0 to 565 in Catalog 2.0. Summit pit craters also have increased, from 173 to 334. Both floor and summit pits are found in similar diameter ranges (5.0-114.0 km vs 5.5-125.4 km, respectively) and locations within the northern hemisphere. Fig. 1 suggests that more central pit craters are found in the heavily cratered highlands regions of the northern hemisphere. But when we divide the planet into 10° latitude by 10° longitude blocks and normalize the number of pit craters to the total number of craters within each region, we find very few locations where pit frequencies exceed 10%. Fig. 2 shows the locations where floor pit craters exceed 10% concentration—these results suggest that floor pits occur preferentially on volcanic units, perhaps because of the layered nature of these regions." @default.
• W1553006072 created "2016-06-24" @default.
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• W1553006072 date "2010-03-01" @default.
• W1553006072 modified "2023-09-23" @default.
• W1553006072 title "Central Pit, Central Peak, and Elliptical Craters in the Martian Northern Hemisphere: New Results from the Revised Catalog of Large Martian Impact Craters" @default.
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