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The precise mechanisms by which martian hillside gullies erode and their dependence on the local environment remain subjects of debate. We studied three sharp rimmed craters in Noachis Terra and 37 gully profiles using Context Camera (CTX), Mars Orbiter Laser Altimeter (MOLA) and High Resolution Stereo Camera (HRSC) data. We analysed the gully topographic profiles of seven gullies and nine dry ravines. We measured slope properties using HRSC elevation data and used thermal inertia to infer material types of the gully sites. We compared these with three nearby Noachian age craters possessing crater wall slope angles within the range of previously observed gully formations. In-line with previous findings on individual gullies, we found that the slope angles of gullies in our study area consistently reflect the inherited slope angles of the host escarpment, suggesting that traditional slope-based evidence of fluvial activity in martian gullies needs to be placed in context of its local environment. We also observed a direct relationship between gully morphology and local composition of surface units. Martian gully features, and possibly method of erosion appeared heavily influenced by changes in underlying geology and presence of erodible sediment. Examples included gully shape changing in accordance with type of erodible sediment. We suggest that the degraded rims of gully-free Noachian craters precluded slope angles high enough to trigger creation of precursors to alcoves through mass wasting. Lack of these hollows has probably prevented the accumulation of enough ice-rich sediment for gullies to form in. Our analysis reveals that there is a complex interdependence between slope processes and the local environment, and global martian gully models may not work at the local scale. [ABSTRACT FROM AUTHOR]

Abstract: Comparison of Martian hillside gullies with terrestrial analogues is a productive method for gaining an understanding of how surface processes operate on Mars and on Earth as well as their similarities and differences. Here we compare gullies within a semiarid region of Island Lagoon near Woomera, Australia, and periglacial gullies located at Pasture Hill, New Zealand, with the Martian gullies in Noachis Terra. We discovered that fluvial processes dominate erosion at the terrestrial sites, though in different forms. Concentration of overland flow and the presence of a resistant cap rock have played a key role in the location and shape of the Island Lagoon gullies. The presence of steeper slopes and a greater abundance of volatiles such as water, frost, and snowmelt at Pasture Hill have helped carve channels equivalent in size to the Martian gullies; and the interaction of frost, dry flows, snowmelt, and debris flows has led to a complex regime of gully erosion and deposition. The observation of similar features on Mars suggests that Martian gully formation is not necessarily restricted to a single process. In addition, gully slopes are closely related to those of their host escarpment as well as the thickness of erodible material and presence of bedrock. Traditional indicators of water-related activity such as slope and sinuosity need to be placed into the context of the environment of the study site. [Copyright &y& Elsevier]

Abstract: Terrestrial gullies provide a useful benchmark to compare martian gully forms against. We compare pole and equator facing gullies in an unnamed crater located in the martian southern mid-latitudes with gullies located on the Lake George escarpment south of Gearys Gap, New South Wales, Australia. Our investigations showed gully morphology at both sites is greatly influenced by thickness of readily erodable regolith, local slope and the presence or absence of bedrock exposures in the gullies. We found that the martian pole-facing gullies are the most similar to those of Lake George and both systems are therefore likely to have been eroded by liquid water. Although the martian gullies possessed much greater volumes of eroded sediment, they had not eroded to underlying bedrock. This contrasts with the smaller Lake George gully channels where numerous bedrock exposures, observed during our survey, affected their slope and overall morphology. Similarly, although dominated by dry processes, multiple bedrock exposures are present within the equator facing martian gullies affecting their cross sectional area and hence sediment transport. The studied sites all showed significant influence from initial slope angles, indicating that interpretation of gully forms such as slopes below the angle of repose, curved profiles and sinuosity must be placed in context of local environments. This analysis can be applied to other regions of Mars and Earth and provide a greater understanding of how geomorphologic processes operate on both worlds. [Copyright &y& Elsevier]

Abstract: The study of hillslopes is a primary element of geomorphology and has successfully been used in many terrestrial arenas. In this study we take advantage of High Resolution Imaging Science Experiment (HiRISE) imagery as well as Mars Orbiter Camera (MOC) derived DEMs of the Pathfinder landing site to study regional hillslopes at resolutions many times greater than previously available and compare them with Mars Pathfinder lander images. This site was thought to be modified by massive flooding 1.8–3.5byr ago and although evidence of flood activity was not obvious at the finer scale of this study, possible lee deposits and terracing were seen in some of the features. Evidence of post flood processes of ice related creep, aeolian and dry mass wasting were observed at the site and have likely obscured flood related morphology present in these features. Regional slopes were found to vary with aspect and suggest processes intensities operating at different orientations, possibly related to the prevailing wind direction, as well as the origin of the ancient flood event. [Copyright &y& Elsevier]

Astronauts working on the surface of Mars have the capability to explore efficiently, rapidly, and flexibly, allowing them to perform a wide range of field investigations. NASA has begun an open international process to identify and evaluate candidate locations where crews could land, live and work on the martian surface, beginning with the First Landing Site/Exploration Zone Workshop for Human Missions to the Surface of Mars in October 2015. Forty seven sites were proposed, including several at or near the Meridiani area, the subject of this paper. We consider the Meridiani area an excellent candidate for the first missions to Mars. It is accessible, safe, contains potential water resources in the form of poly-hydrated magnesium sulphates, has diverse science features with high likelihood of meeting all science goals, has other potential resources and potential for further longer-ranged exploration. The presence of hardware from previous missions will be of benefit to studies of materials to martian conditions, assessing the effectiveness of historic planetary protection strategies, and engaging public interest. Lastly, parts of the Meridiani region have been well studied from the surface by the Opportunity mission, providing ground truth for orbital data. As one of the best documented regions of Mars this will allow a “Go where you know” approach for the first crewed missions, especially with regard to safety, trafficability, and water resource potential. [ABSTRACT FROM AUTHOR]