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![1: The Martian surface with prominent features marked including Arabia Terra. The north-central section of Arabia Terra is the region of study for this project [Image credit: NASA].](profile/Michael-Zeilnhofer/publication/323880550/figure/fig11/AS:626936225230856@1526484652737/The-Martian-surface-with-prominent-features-marked-including-Arabia-Terra-The.png)
1: The Martian surface with prominent features marked including Arabia Terra. The north-central section of Arabia Terra is the region of study for this project [Image credit: NASA].
Source publication
The results from this study show that during the middle Amazonian period (2 Ga), Arabia Terra did exhibit glacial and fluvial activity as predicted by the Global Circulation Model. Arabia Terra is the largest expanse of ancient terrain north of the Martian equator. Arabia Terra extends across the Martian prime meridian from approximately 30°E (330°...
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... largest expanse of ancient terrain north of the Martian equator is Arabia Figure 2.1] covers ∼ 12x10 6 km 2 in area and contains material from the oldest time period on Mars, the Noachian period [ Anguita et al., 1997]. ...
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... topography of Arabia Terra has been defined using Mars Orbiter Laser Altimeter (MOLA) [ Figure 2.2]. Compared to the rest of the cratered terrain where elevations range from +1 km to + 4 km, Arabia Terra has elevations which range from -3 km to + 1 km [Evans et al., 2010]. ...
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... Terra is also an area of interest due to past studies on the elements found in the rocks. The Gamma Ray Spectrometer (GRS) aboard Mars Odyssey revealed that Arabia Terra has an elevated hydrogen content ranging between 5 and 7 wt%, as well as a large equivalent water content (5.7 wt%) [ Figure 2.3] compared to the 3.9 wt% equivalent water content global average for non-polar regions. ...
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... looking at the crater morphologies of Arabia Terra there is an abundance (12%) of craters which display multiple layered ejecta (MLE) (three or more par- tial or complete ejecta layers) [ Barlow et al., 2000] which is intriguing because of all the craters on Mars only 5% are MLE [Barlow and Perez, 2003]. Other ejecta mor- phologies seen [ Figure 2.4] in Arabia Terra are single layer ejecta (SLE) and double layer ejecta (DLE). Single layer ejecta displays one ejecta layer and a double layer ejecta has two complete ejecta layers [ Barlow et al., 2000]. ...
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... wind transports the loose grains of dust and sand, depositing them into the basins of impact craters. Sand dunes (SD) [ Figure 2.5a] are a very common interior morphology which is seen all over the surface of Mars [Kok, 2009]. ...
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... craters also exhibit dark streaks along the steep slopes of crater walls and central peaks. These streaks are dust avalanches (DA) [ Figure 2.5b], caused by downslope movement of dust which uncovers darker, underlying material (larger grains or bedrock) [Chuang et al., 2010]. ...
