Geomorphological Analysis of ExoMars Candidate Landing Site Oxia Planum

Иванов, М. А.; Slyuta, E. N.; Grishakina, E. A.; Dmitrovskii, A. A.

doi:10.1134/s0038094620010050

Cited by 29 publications

(29 citation statements)

References 29 publications

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“…Ivanov et al. (2020) mapped the Oxia region using CTX data and obtained crater retention ages for some of their mapped units; their unit “lbp (light plains)” and “ups (smooth highland plains)” roughly correspond with the western and eastern subsections of our Unit 1. For the lbp and ups units, they report crater retention ages of ∼3.5 Ga and ∼3.65 Ga, respectively.…”

Section: Resultsmentioning

confidence: 99%

Geologic and Thermal Characterization of Oxia Planum Using Mars Odyssey THEMIS Data

Gary‐Bicas

Rogers

2021

JGR Planets

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is a region on Mars located southeast of Chryse Planitia and west of Arabia Terra, at the transitional boundary between the cratered highlands and lowland plains. It lies between two of the largest channel features on Mars, Ares Vallis, and Mawrth Vallis (Figures 1a and 1b). Previous studies that examined the crater size frequency distribution across the region suggest a crater retention age between 3.7 and 3.9 Ga, near the late Noachian/early Hesperian boundary (Tanaka et al. 2014). Previous geomorphological assessments noted fans and channel deposits that indicate evidence of past aqueous activity (Molina et al., 2017). Mineralogical studies done on this region have been conducted using shortwave infrared (SWIR, 1.0-2.6 μm) spectral data from the Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité (OMEGA)

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Section: Resultsmentioning

confidence: 99%

Geologic and Thermal Characterization of Oxia Planum Using Mars Odyssey THEMIS Data

Gary‐Bicas

Rogers

2021

JGR Planets

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“…Craters are considered as possible hazards in the landing‐site evaluation due to their internal slopes and protuberant rims (Brady et al., 2009), especially for relatively young craters (Erkeling et al., 2012; Ivanov et al., 2020; Pajola, Rossato, Carter, et al., 2016). The more the craters are distributed in a region, the more dangerous is the terrain surface, which will reduce the flexibility in hazard avoidance during the descent phase of the lander.…”

Section: Geomorphological Characteristics Of the Candidate Landing Regionmentioning

confidence: 99%

Characterization of the Candidate Landing Region for Tianwen‐1—China's First Mission to Mars

Dong

Wang

et al. 2021

Earth and Space Science

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This paper presents our efforts to characterize the candidate landing region (109°–133°E, 23°–30°N) for Tianwen‐1, China's first mission to Mars, in terms of engineering safety and scientific significance. Topographic analysis reveals that the region has a low elevation around −4,230 m, and 98% of the region have slopes smaller than 8°. The geomorphological mapping and analysis show that the region has an average crater density of about 28 craters (≥200 m in diameter) per 100 square kilometers, with several clusters of high crater densities distributed around the center of the region. There are also pitted cones distributed mainly in the southern part of the region, with a density of approximately 6.6 cones per 100 square kilometers in specific local areas. The region has rock abundances ranging from 1% to 23%, with local clusters of low and high rock abundances. The region comprises four main geological units, including a lowland unit formed in the Late Hesperian and a volcanic unit formed in the Amazonian and Hesperian period. Their specific surface ages are estimated through the analysis of crater size‐frequency distribution. Combining the engineering constraints on surface slopes, crater density, cone density, and rock abundance, a hazard map of the candidate landing region is generated for landing site evaluation and safety assessment. Based on the results, we further discuss the potential scientific outcomes from the exploration in this region. The findings will be helpful for the mission planning and maximization of the scientific return from Tianwen‐1, and complement existing Martian scientific research.

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“…18A, 18B) and a polygonally fractured geomorphic expression ( Fig. 18B; Parkes Bowen et al, 2019;Ivanov et al, 2020), and it contains clay minerals (Carter et al, 2016;Molina et al, 2017). The fracture pattern, the scale of the fracture pattern, and the crater retention properties of this rock (Fig.…”

Section: Research Papermentioning

confidence: 95%

“…to explore a record that includes deltaic sediment deposited at the terminus of the Coogoon Vallis fluvial system (Molina et al, 2017;Fawdon et al, 2019;Ivanov et al, 2020). These sediments might or might not be accessed by the rover, depending on exactly where it lands, where the science team decides to drive the rover, and how much time is available for exploration of the area.…”

Section: Research Papermentioning

confidence: 99%

Extraformational sediment recycling on Mars

et al. 2020

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Extraformational sediment recycling (old sedimentary rock to new sedimentary rock) is a fundamental aspect of Earth’s geological record; tectonism exposes sedimentary rock, whereupon it is weathered and eroded to form new sediment that later becomes lithified. On Mars, tectonism has been minor, but two decades of orbiter instrument–based studies show that some sedimentary rocks previously buried to depths of kilometers have been exposed, by erosion, at the surface. Four locations in Gale crater, explored using the National Aeronautics and Space Administration’s Curiosity rover, exhibit sedimentary lithoclasts in sedimentary rock: At Marias Pass, they are mudstone fragments in sandstone derived from strata below an erosional unconformity; at Bimbe, they are pebble-sized sandstone and, possibly, laminated, intraclast-bearing, chemical (calcium sulfate) sediment fragments in conglomerates; at Cooperstown, they are pebble-sized fragments of sandstone within coarse sandstone; at Dingo Gap, they are cobble-sized, stratified sandstone fragments in conglomerate derived from an immediately underlying sandstone. Mars orbiter images show lithified sediment fans at the termini of canyons that incise sedimentary rock in Gale crater; these, too, consist of recycled, extraformational sediment. The recycled sediments in Gale crater are compositionally immature, indicating the dominance of physical weathering processes during the second known cycle. The observations at Marias Pass indicate that sediment eroded and removed from craters such as Gale crater during the Martian Hesperian Period could have been recycled to form new rock elsewhere. Our results permit prediction that lithified deltaic sediments at the Perseverance (landing in 2021) and Rosalind Franklin (landing in 2023) rover field sites could contain extraformational recycled sediment.

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Geomorphological Analysis of ExoMars Candidate Landing Site Oxia Planum

Cited by 29 publications

References 29 publications

Geologic and Thermal Characterization of Oxia Planum Using Mars Odyssey THEMIS Data

Geologic and Thermal Characterization of Oxia Planum Using Mars Odyssey THEMIS Data

Characterization of the Candidate Landing Region for Tianwen‐1—China's First Mission to Mars

Extraformational sediment recycling on Mars

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