Mars: Abundant Recurring Slope Lineae (RSL) Following the Planet‐Encircling Dust Event (PEDE) of 2018

McEwen, A. S.; Schaefer, E. I.; Dundas, C. M.; Sutton, Sarah; Tamppari, L. K.; Chojnacki, M.

doi:10.1029/2020je006575

Cited by 26 publications

(13 citation statements)

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“…The slopes here host Recurring Slope Lineae (RSL) and gullies. RSL are dark linear markings that grow downslope during the warmest periods of the year and were initially thought to be liquid water seeps, e.g., [42][43][44], although that interpretation has been overturned and re-established many times over in the last decade, e.g., [45][46][47][48][49][50]. The southern edge of the central peak area is bounded by dark aeolian dunes.…”

Section: Study Sitesmentioning

confidence: 99%

Single Image Super-Resolution Restoration of TGO CaSSIS Colour Images: Demonstration with Perseverance Rover Landing Site and Mars Science Targets

et al. 2021

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The ExoMars Trace Gas Orbiter (TGO)’s Colour and Stereo Surface Imaging System (CaSSIS) provides multi-spectral optical imagery at 4-5m/pixel spatial resolution. Improving the spatial resolution of CaSSIS images would allow greater amounts of scientific information to be extracted. In this work, we propose a novel Multi-scale Adaptive weighted Residual Super-resolution Generative Adversarial Network (MARSGAN) for single-image super-resolution restoration of TGO CaSSIS images, and demonstrate how this provides an effective resolution enhancement factor of about 3 times. We demonstrate with qualitative and quantitative assessments of CaSSIS SRR results over the Mars2020 Perseverance rover’s landing site. We also show examples of similar SRR performance over 8 science test sites mainly selected for being covered by HiRISE at higher resolution for comparison, which include many features unique to the Martian surface. Application of MARSGAN will allow high resolution colour imagery from CaSSIS to be obtained over extensive areas of Mars beyond what has been possible to obtain to date from HiRISE.

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Section: Study Sitesmentioning

confidence: 99%

Single Image Super-Resolution Restoration of TGO CaSSIS Colour Images: Demonstration with Perseverance Rover Landing Site and Mars Science Targets

et al. 2021

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“…Many hundreds of possible and confirmed RSL sites have been mapped, primarily in the southern midlatitudes, Valles Marineris, and Chryse and Acidalia Planitiae (Stillman, 2018; Stillman & Grimm, 2018; Stillman et al., 2014, 2016, 2017; McEwen et al., 2021; Ojha et al., 2014). RSL are generally active in warm seasons (McEwen et al., 2011, 2014; Ojha et al., 2014; Stillman et al., 2014), and they were more active and widespread immediately following planet‐encircling dust events (PEDEs) (McEwen et al., 2011, 2021; Stillman et al., 2014). Some lineae have similar morphology but different temporal behavior (e.g., Dundas, 2020a; McEwen et al., 2014).…”

Section: Mass Wasting and Slope Processesmentioning

confidence: 99%

“…They characteristically exhibit incremental growth over a period of several months, fade annually, and recur in approximately the same locations. Many hundreds of possible and confirmed RSL sites have been mapped, primarily in the southern midlatitudes, Valles Marineris, and Chryse and Acidalia Planitiae (Stillman, 2018;Stillman & Grimm, 2018;Stillman et al, 2014Stillman et al, , 2016Stillman et al, , 2017McEwen et al, 2021;Ojha et al, 2014). RSL are generally active in warm seasons (McEwen et al, 2011(McEwen et al, , 2014Ojha et al, 2014;Stillman et al, 2014), and they were more active and widespread immediately following planet-encircling dust events (PEDEs) DUNDAS ET AL.…”

Section: Rsl and Slumpsmentioning

confidence: 99%

“…10.1029/2021JE006876 12 of 35 ( McEwen et al, 2011McEwen et al, , 2021Stillman et al, 2014). Some lineae have similar morphology but different temporal behavior (e.g., Dundas, 2020a;McEwen et al, 2014).…”

Section: Rsl and Slumpsmentioning

confidence: 99%

“…More recently, Schaefer et al (2019) and Vincendon et al (2019) proposed entirely dry hypotheses for RSL formation involving mobilization of surface dust, while Dundas (2020a) argued that they are aeolian-driven sand flows made visible by the absence of a dust coating on fresh flows. The great abundance of RSL and associated dust devil tracks following the 2018 PEDE suggest that dust lifting may initiate RSL formation (McEwen et al, 2021). Chojnacki et al (2016) and Ojha et al (2017) described slumps occurring at some RSL sites in Valles Marineris.…”

Section: Journal Of Geophysical Research: Planetsmentioning

confidence: 99%

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Active Mars: A Dynamic World

et al. 2021

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An axiom of geology is that the present is the key to the past. Knowledge of current processes and their consequences is an essential tool for understanding history, including the ancient rock record and the associated climate. Modern Mars is cold, with a thin atmosphere, and has previously been thought to have little ongoing geomorphic activity-especially when compared with ancient Mars, which had apparent largescale, Earth-like processes, as inferred from ancient landforms. This interpretation has led much research to focus not on the present Martian environment, but rather on Mars' early conditions and climate change over time. However, in recent years, observations of ongoing surface changes have proliferated, demonstrating that Mars' landscape is actively evolving and likely has been throughout the Amazonian epoch. These observed geomorphic changes shed light on a variety of active processes, some with no terrestrial analog, and reveal present-day Mars to be a dynamic world. This in turn may mean that more of the ancient and recent Martian geologic record can be explained without dramatic climate change.This work presents a comprehensive summary and categorization of the many types of observed changes on the Martian surface. Aeolian and frost-related surface activity are discussed in more detail in a parallel review by Diniega et al. (2021), which focuses on connecting specific landforms to their formative processes; the focus herein is to provide a broad overview of known types of changes in surface morphology and albedo. Weather and seasonal frost and ice are not discussed in detail here, except where necessary to describe their effects on the surface; observations of the atmosphere were reviewed by M. D. Smith (2008) and Martínez et al. (2017), and seasonal frost is discussed in Piqueux, Kleinböhl, et al. (2015) and references therein. Weathering and other microscale or chemical processes are not discussed. Even with these exclusions, the scope of the subject is broad and we have focused on the key discoveries and constraints.Studying surface changes on Mars yields a unique look at processes within an un-Earthly environment.

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Sedimentary Processes on Venus

Carter,

Gilmore,

Ghail

et al. 2023

Space Sci Rev

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The sedimentary cycle, including the processes of erosion, transport, and lithification, is a key part of how planets evolve over time. Early images of Venus’s vast volcanic plains, numerous volcanoes, and rugged tectonic regions led to the interpretation that Venus is a volcanic planet with little sediment cover and perhaps few processes for generating sedimentary rocks. However, in the years since the Magellan mission in the 1990s we have developed a better understanding of sedimentary process on Venus. Impact craters are the largest present-day source of sediments, with estimates from the current crater population suggesting an average sediment layer 8–63 cm in thickness if distributed globally. There is clear evidence of fine-grained material in volcanic summit regions that is likely produced through volcanism, and dune fields and yardangs indicate transport of sediments and erosion of rocks through wind. Landslides and fine-grained materials in highland tessera regions demonstrate erosive processes that move sediment downhill. It is clear that sediments are an important part of Venus’s geology, and it is especially important to realize that they mantle features that may be of interest to future landed or low-altitude imaging missions. The sinks of sediments are less well known, as it has been difficult to identify sedimentary rocks with current data. Layering observed in Venera images and in Magellan images of some tessera regions, as well as calculated rock densities, suggest that sedimentary rocks are present on Venus. New data is needed to fully understand and quantify the present-day sedimentary cycle and establish with certainty whether sedimentary rock packages do, in fact, exist on Venus. These data sets will need to include higher-resolution optical and radar imaging, experimental and geochemical measurements to determine how chemical weathering and lithification can occur, and topography to better model mesospheric winds. Sediments and sedimentary rocks are critical to understanding how Venus works today, but are also extremely important for determining how Venus’s climate has changed through time and whether it was once a habitable planet.

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Mars: Abundant Recurring Slope Lineae (RSL) Following the Planet‐Encircling Dust Event (PEDE) of 2018

Cited by 26 publications

References 90 publications

Single Image Super-Resolution Restoration of TGO CaSSIS Colour Images: Demonstration with Perseverance Rover Landing Site and Mars Science Targets

Single Image Super-Resolution Restoration of TGO CaSSIS Colour Images: Demonstration with Perseverance Rover Landing Site and Mars Science Targets

Active Mars: A Dynamic World

Sedimentary Processes on Venus

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