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• W287446255 abstract "Introduction: Impact cratering is arguably the most important surficial geologic process occurring on the terrestrial planets (with the exception of Earth). Since impact craters can be considered closed systems, they are excellent tools for measuring the degree and type of erosion occurring on a planet’s surface. Until recently, studying the geomorphic features of impact craters on Mars has been difficult due to poor data resolution. However, within the last decade, the Mars Orbiter Laser Altimeter (MOLA) has returned high resolution topographic data of the Martian surface. Using these data and images of Mars returned from the Viking missions, we have created a comprehensive database of degradational characteristics of the craters in the Sinus Sabaeus region of Mars. The purpose of this study is to gain a better understanding of the past and present surface processes that modify the surface topography of Mars. Site Description: The Sinus Sabaeus region of Mars covers an area approximately bounded by 0N and 30S latitude, and 315W and 360W longitude. Located in the southern highlands, this area is heavily cratered and Noachian in age [1]. Sinus Sabaeus is topographically fairly homogenous. Thermal inertia measurements of the area indicate that the surface is covered by a thick layer of sand-sized to fine-grained sediments, inferred to be the result of eolian deposition. Mars Orbiter Camera (MOC) images have shown that the layer of sediment varies in thickness from location to location in the region. The rock abundance of the region has been estimated to be less than or equal to 10% [2,3,4]. Data Sets and Methods: In this study, we have used both imagery and topographic data to collect information about the craters. The images of Mars were collected by the Viking Orbiter missions (MDIMs) and have a resolution of at least 400m/pixel. Each covers an area of approximately 5 degrees latitude by 5 degrees longitude. The second dataset used consists of topographic data collected by MOLA and has a nominal vertical resolution of approximately 0.5m and a horizontal resolution of approximately 330 m [5]. The resolution of this data is approximately 1 km, although the spacing between the tracks was essentially random, so some gaps of several kilometers between tracks have occurred. Craters larger than 10 km in diameter were chosen for this study due to the resolution limitations of the MOLA data. Each crater was studied both qualitatively and quantitatively. Using the MDIMs, crater degradation levels were estimated visually using a classification scheme developed in Craddock, et al. [6]. Degradation classes ranged from Type A, referring to very fresh craters (with central peaks, sharp rims and ejecta blankets), to Type E, referring to the most degraded craters (with no rim and an irregular floor). For each crater chosen for study, a topographic map was created using the MOLA data. From this map, the crater’s geometric center, lowest elevation region and rim boundaries were located using the program Surfer (Figure 1). This information was then inputted into a FORTRAN program that accessed all of the raw topographic data for the crater out to a distance of two crater diameters from the center. Within the FORTRAN program, each crater was divided into eight equal 45-degree sectors. Information was averaged within each sector. This information was used to calculate values such as average depth, rim diameter, rim height, floor diameter and maximum wall slope of the crater." @default.
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• W287446255 date "2003-03-01" @default.
• W287446255 modified "2023-09-24" @default.
• W287446255 title "Observations on Spatial Relationships of Impact Crater Floor Morphologies in the Sinus Sabaeus Region of Mars" @default.
• W287446255 hasPublicationYear "2003" @default.
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