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Academic literature on the topic 'Mars craters'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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Journal articles on the topic "Mars craters"

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Francis, Alistair, Jonathan Brown, Thomas Cameron, Reuben Crawford Clarke, Romilly Dodd, Jennifer Hurdle, Matthew Neave, et al. "A Multi-Annotator Survey of Sub-km Craters on Mars." Data 5, no. 3 (August 3, 2020): 70. http://dx.doi.org/10.3390/data5030070.

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We present here a dataset of nearly 5000 small craters across roughly 1700 km2 of the Martian surface, in the MC-11 East quadrangle. The dataset covers twelve 2000-by-2000 pixel Context Camera images, each of which is comprehensively labelled by six annotators, whose results are combined using agglomerative clustering. Crater size-frequency distributions are centrally important to the estimation of planetary surface ages, in lieu of in-situ sampling. Older surfaces are exposed to meteoritic impactors for longer and, thus, are more densely cratered. However, whilst populations of larger craters are well understood, the processes governing the production and erosion of small (sub-km) craters are more poorly constrained. We argue that, by surveying larger numbers of small craters, the planetary science community can reduce some of the current uncertainties regarding their production and erosion rates. To this end, many have sought to use state-of-the-art object detection techniques utilising Deep Learning, which—although powerful—require very large amounts of labelled training data to perform optimally. This survey gives researchers a large dataset to analyse small crater statistics over MC-11 East, and allows them to better train and validate their crater detection algorithms. The collection of these data also demonstrates a multi-annotator method for the labelling of many small objects, which produces an estimated confidence score for each annotation and annotator.

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Zimbelman, James R., and Stephen P. Scheidt. "Hesperian Age for Western Medusae Fossae Formation, Mars." Science 336, no. 6089 (May 24, 2012): 1683. http://dx.doi.org/10.1126/science.1221094.

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The Medusae Fossae Formation (MFF) on Mars is an intensely eroded deposit north of the cratered highlands. It is widely thought that MFF materials were emplaced through ignimbrite eruptions. Recent geologic mapping of western MFF identified outliers of MFF materials well beyond the previously mapped western extent for the deposit, including outliers close to Gale crater. We report counts of impact craters on the MFF units that have implications for our understanding of the general history of MFF and the uppermost layered materials on the Gale crater mound.

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Hardy, Stuart. "Discrete Element Modelling of Pit Crater Formation on Mars." Geosciences 11, no. 7 (June 24, 2021): 268. http://dx.doi.org/10.3390/geosciences11070268.

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Pit craters are now recognised as being an important part of the surface morphology and structure of many planetary bodies, and are particularly remarkable on Mars. They are thought to arise from the drainage or collapse of a relatively weak surficial material into an open (or widening) void in a much stronger material below. These craters have a very distinctive expression, often presenting funnel-, cone-, or bowl-shaped geometries. Analogue models of pit crater formation produce pits that typically have steep, nearly conical cross sections, but only show the surface expression of their initiation and evolution. Numerical modelling studies of pit crater formation are limited and have produced some interesting, but nonetheless puzzling, results. Presented here is a high-resolution, 2D discrete element model of weak cover (regolith) collapse into either a static or a widening underlying void. Frictional and frictional-cohesive discrete elements are used to represent a range of probable cover rheologies. Under Martian gravitational conditions, frictional-cohesive and frictional materials both produce cone- and bowl-shaped pit craters. For a given cover thickness, the specific crater shape depends on the amount of underlying void space created for drainage. When the void space is small relative to the cover thickness, craters have bowl-shaped geometries. In contrast, when the void space is large relative to the cover thickness, craters have cone-shaped geometries with essentially planar (nearing the angle of repose) slope profiles. Frictional-cohesive materials exhibit more distinct rims than simple frictional materials and, thus, may reveal some stratigraphic layering on the pit crater walls. In an extreme case, when drainage from the overlying cover is insufficient to fill an underlying void, skylights into the deeper structure are created. This study demonstrated that pit crater walls can exhibit both angle of repose slopes and stable, gentler, collapse slopes. In addition, the simulations highlighted that pit crater depth only provides a very approximate estimate of regolith thickness. Cone-shaped pit craters gave a reasonable estimate (proxy) of regolith thickness, whereas bowl-shaped pit craters provided only a minimum estimate. Finally, it appears that fresh craters with distinct, sharp rims like those seen on Mars are only formed when the regolith had some cohesive strength. Such a weakly cohesive regolith also produced open fissures, cliffs, and faults, and exposed regolith “stratigraphy” in the uppermost part of the crater walls.

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Jia, Yutong, Gang Wan, Lei Liu, Jue Wang, Yitian Wu, Naiyang Xue, Ying Wang, and Rixin Yang. "Split-Attention Networks with Self-Calibrated Convolution for Moon Impact Crater Detection from Multi-Source Data." Remote Sensing 13, no. 16 (August 12, 2021): 3193. http://dx.doi.org/10.3390/rs13163193.

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Impact craters are the most prominent features on the surface of the Moon, Mars, and Mercury. They play an essential role in constructing lunar bases, the dating of Mars and Mercury, and the surface exploration of other celestial bodies. The traditional crater detection algorithms (CDA) are mainly based on manual interpretation which is combined with classical image processing techniques. The traditional CDAs are, however, inefficient for detecting smaller or overlapped impact craters. In this paper, we propose a Split-Attention Networks with Self-Calibrated Convolution (SCNeSt) architecture, in which the channel-wise attention with multi-path representation and self-calibrated convolutions can generate more prosperous and more discriminative feature representations. The algorithm first extracts the crater feature model under the well-known target detection R-FCN network framework. The trained models are then applied to detecting the impact craters on Mercury and Mars using the transfer learning method. In the lunar impact crater detection experiment, we managed to extract a total of 157,389 impact craters with diameters between 0.6 and 860 km. Our proposed model outperforms the ResNet, ResNeXt, ScNet, and ResNeSt models in terms of recall rate and accuracy is more efficient than that other residual network models. Without training for Mars and Mercury remote sensing data, our model can also identify craters of different scales and demonstrates outstanding robustness and transferability.

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Hsu, Chia-Yu, Wenwen Li, and Sizhe Wang. "Knowledge-Driven GeoAI: Integrating Spatial Knowledge into Multi-Scale Deep Learning for Mars Crater Detection." Remote Sensing 13, no. 11 (May 28, 2021): 2116. http://dx.doi.org/10.3390/rs13112116.

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This paper introduces a new GeoAI solution to support automated mapping of global craters on the Mars surface. Traditional crater detection algorithms suffer from the limitation of working only in a semiautomated or multi-stage manner, and most were developed to handle a specific dataset in a small subarea of Mars’ surface, hindering their transferability for global crater detection. As an alternative, we propose a GeoAI solution based on deep learning to tackle this problem effectively. Three innovative features are integrated into our object detection pipeline: (1) a feature pyramid network is leveraged to generate feature maps with rich semantics across multiple object scales; (2) prior geospatial knowledge based on the Hough transform is integrated to enable more accurate localization of potential craters; and (3) a scale-aware classifier is adopted to increase the prediction accuracy of both large and small crater instances. The results show that the proposed strategies bring a significant increase in crater detection performance than the popular Faster R-CNN model. The integration of geospatial domain knowledge into the data-driven analytics moves GeoAI research up to the next level to enable knowledge-driven GeoAI. This research can be applied to a wide variety of object detection and image analysis tasks.

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Chen, Zihao, and Jie Jiang. "Crater Detection and Recognition Method for Pose Estimation." Remote Sensing 13, no. 17 (September 1, 2021): 3467. http://dx.doi.org/10.3390/rs13173467.

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A crater detection and recognition algorithm is the key to pose estimation based on craters. Due to the changing viewing angle and varying height, the crater is imaged as an ellipse and the scale changes in the landing camera. In this paper, a robust and efficient crater detection and recognition algorithm for fusing the information of sequence images for pose estimation is designed, which can be used in both flying in orbit around and landing phases. Our method consists of two stages: stage 1 for crater detection and stage 2 for crater recognition. In stage 1, a single-stage network with dense anchor points (dense point crater detection network, DPCDN) is conducive to dealing with multi-scale craters, especially small and dense crater scenes. The fast feature-extraction layer (FEL) of the network improves detection speed and reduces network parameters without losing accuracy. We comprehensively evaluate this method and present state-of-art detection performance on a Mars crater dataset. In stage 2, taking the encoded features and intersection over union (IOU) of craters as weights, we solve the weighted bipartite graph matching problem, which is matching craters in the image with the previously identified craters and the pre-established craters database. The former is called “frame-frame match”, or FFM, and the latter is called “frame-database match”, or FDM. Combining the FFM with FDM, the recognition speed is enabled to achieve real-time on the CPU (25 FPS) and the average recognition precision is 98.5%. Finally, the recognition result is used to estimate the pose using the perspective-n-point (PnP) algorithm and results show that the root mean square error (RMSE) of trajectories is less than 10 m and the angle error is less than 1.5 degrees.

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Barata, T., E. I. Alves, A. Machado, and G. A. Barberes. "Characterization of palimpsest craters on Mars." Planetary and Space Science 72, no. 1 (November 2012): 62–69. http://dx.doi.org/10.1016/j.pss.2012.09.015.

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Edgett, Kenneth S., Steven G. Banham, Kristen A. Bennett, Lauren A. Edgar, Christopher S. Edwards, Alberto G. Fairén, Christopher M. Fedo, et al. "Extraformational sediment recycling on Mars." Geosphere 16, no. 6 (October 6, 2020): 1508–37. http://dx.doi.org/10.1130/ges02244.1.

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Abstract 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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Carporzen, Laurent, Stuart A. Gilder, and Rodger J. Hart. "Palaeomagnetism of the Vredefort meteorite crater and implications for craters on Mars." Nature 435, no. 7039 (May 2005): 198–201. http://dx.doi.org/10.1038/nature03560.

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MCEWEN, A., B. PREBLICH, E. TURTLE, N. ARTEMIEVA, M. GOLOMBEK, M. HURST, R. KIRK, D. BURR, and P. CHRISTENSEN. "The rayed crater Zunil and interpretations of small impact craters on Mars." Icarus 176, no. 2 (August 2005): 351–81. http://dx.doi.org/10.1016/j.icarus.2005.02.009.

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Dissertations / Theses on the topic "Mars craters"

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De, Villiers Germari Marzen Luke J. King David T. "Remote sensing of shallow-marine impact craters on Mars." Auburn, Ala., 2007. http://hdl.handle.net/10415/1343.

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Kukkonen, S. (Soile). "Small impact craters in crater counting:evolution studies of the eastern Hellas outflow channels, Mars." Doctoral thesis, Oulun yliopisto, 2018. http://urn.fi/urn:isbn:9789526218779.

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Abstract Crater counting is a method which allows us to estimate the surface ages of the planetary bodies, from which the sampling and sample delivery to laboratories on Earth are difficult or impossible. Because the number of craters on a surface unit increases over the time the surface has been exposed to space, old, geologically stable units have more craters than young and active units. When the crater production rate as a function of time is known, the absolute age of the surface unit can be determined based on its crater density. The purpose of this thesis is to investigate the role of small impact craters in crater counts to find out how modern very high-resolution space images can be utilized in age determination of planetary surfaces. The thesis focuses on how reliable crater count based datings are, if only small craters and counting areas are used in age determination. The research is carried out by utilizing crater counts on the outflow channels of Dao, Niger, Harmakhis and Reull Valles, which all are located in the eastern rim region of the Hellas impact basin, on the southern hemisphere of Mars. Crater counts are performed mainly based on the images of ConTeXt Imager (CTX) and High Resolution Imaging Science Experiment (HiRISE) aboard Mars Reconnaissance Orbiter (MRO). The results show that small craters are a very valuable tool to get information about the surface age. Instead of the size-range of counted craters, or the size of counting areas, results are dependent on the variability and scale of the surface modification history. The more variable or larger scale the modification history is, the larger surface area and wider crater diameter range are typically needed to achieve comprehensive age estimations. The crater counts on the eastern Hellas outflow channels support the earlier theories according to which the valles formed during a relatively short time interval, ~ 3.4–3.7 Ga ago. The existence of terrace structures and smaller tributary channels indicate that the outflow channels were filled by several pulses of liquids. The major fluvial activity ended no later than ~ 0.8–1.9 Ga ago, and it was probably controlled by the activity of nearby highland volcanoes. Soon after the declined fluvial activity, the outflow channels were covered by ice-rich deposits. The major reason for this was probably the changed climatic conditions, although in places e.g. impact cratering seems to have contributed to the emplacement of the deposits. The region as a whole was also resurfaced several times because of changes in local climate conditions. The most significant of the resurfacing processes seem to be the episodes of thin ice-rich mantling deposits, the most recent of which dominated the regional modification less than 10 Ma ago. In addition, the region has experienced eolian activity during the last 1 Ma
Original papers The original publications are not included in the electronic version of the dissertation. Kostama, V.-P., Kukkonen, S., & Raitala, J. (2017). Resurfacing event observed in Morpheos basin (Eridania Planitia) and the implications to the formation and timing of Waikato and Reull Valles, Mars. Planetary and Space Science, 140, 35–48. https://doi.org/10.1016/j.pss.2017.04.001 Kukkonen, S., & Kostama, V.-P. (2018). Modification history of the Harmakhis Vallis outflow channel, Mars, based on CTX-scale photogeologic mapping and crater count dating. Icarus, 299, 46–67. https://doi.org/10.1016/j.icarus.2017.07.014 Kukkonen, S., & Kostama, V.-P. (2018). Usability of small impact craters on small surface areas in crater count dating: Analysing examples from the Harmakhis Vallis outflow channel, Mars. Icarus, 305, 33–49. https://doi.org/10.1016/j.icarus.2018.01.004 Kukkonen, S., & Kostama, V.-P. (2018). Mapping and dating based evolution studies of the Niger Vallis outflow channel, Mars. Planetary and Space Science, 153, 54–71. https://doi.org/10.1016/j.pss.2017.12.012 Korteniemi, J., & Kukkonen, S. (2018). Volcanic Structures Within Niger and Dao Valles, Mars, and Implications for Outflow Channel Evolution and Hellas Basin Rim Development. Geophysical Research Letters, 45(7), 2934–2944. https://doi.org/10.1002/2018gl077067 http://jultika.oulu.fi/Record/nbnfi-fe201902226008

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Chee, Yenlai. "Remote sensing analysis of cratered surfaces Mars landing hazard assessment, comparison to terrestrial crater analogs, and Mars crater dating models /." To access this resource online via ProQuest Dissertations and Theses @ UTEP, 2007. http://0-proquest.umi.com.lib.utep.edu/login?COPT=REJTPTU0YmImSU5UPTAmVkVSPTI=&clientId=2515.

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BARLOW, NADINE GAIL. "RELATIVE AGES AND THE GEOLOGIC EVOLUTION OF MARTIAN TERRAIN UNITS (MARS, CRATERS)." Diss., The University of Arizona, 1987. http://hdl.handle.net/10150/184013.

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Existing martian relative age chronologies rely entirely or predominantly on Mariner 9 images, extrapolated numbers of craters, and craters 500(DEGREES)K) for the planet are consistent with the derived chronology.

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Daubar, Ingrid Justine. "New Dated Craters On Mars And The Moon: Studies Of The Freshest Craters In The Solar System." Diss., The University of Arizona, 2014. http://hdl.handle.net/10150/337303.

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New, dated impacts discovered on Mars and the Moon provide direct observations of modern bombardment in the inner Solar System and the freshest available examples of recent craters. Their population, morphology, formation and modification processes relate to issues with secondaries and help calibrate cratering chronology models. I use a subset of the new impacts to measure the current production function at Mars. The resulting production function is a factor of approximately four lower than widely-used models, and the size frequency distribution has a shallower slope. This discrepancy between the measured current impact flux and model predictions could be due to many issues, so craters <~50m diameter should not be used for crater age dating unless the uncertainties are understood. I find that these new martian craters are only slightly deeper on average than the expected depth/diameter ratio (d/D) of ~0.2 for simple primaries; the majority would not be mistaken for secondaries based on d/D. A wide spread in d/D indicates that impact conditions or target properties might influence final crater morphologies at these sizes. Extended low-albedo features surround these new craters, presumed to have formed when the impact blast disturbed a surface coating of high-albedo dust, exposing a darker substrate. Some of these features changed drastically over a few Mars years, however, half of the sites show no changes at all. Estimated fading lifetimes cluster around ~7 Mars years. Controls on the amount and rates of fading have yet to be determined. These results show that the current impact production function is not under-sampling new impacts due to fading prior to detection. New craters have also been discovered on the Moon, using similar techniques. Five new impact craters were found that formed within the last ~40 years. Conclusions are unreliable with only these scant statistics, but preliminary comparisons indicate they follow the expected size frequency distribution predicted by the Neukum [1983; Neukum et al., 2001] production function and chronology. This also leads to a very preliminary measurement of the current Moon/Mars cratering ratio at a single diameter, which falls below models by only a factor of approximately six.

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Bamberg, Marlene. "Planetary mapping tools applied to floor-fractured craters on Mars." Phd thesis, Universität Potsdam, 2014. http://opus.kobv.de/ubp/volltexte/2014/7210/.

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Planetary research is often user-based and requires considerable skill, time, and effort. Unfortunately, self-defined boundary conditions, definitions, and rules are often not documented or not easy to comprehend due to the complexity of research. This makes a comparison to other studies, or an extension of the already existing research, complicated. Comparisons are often distorted, because results rely on different, not well defined, or even unknown boundary conditions. The purpose of this research is to develop a standardized analysis method for planetary surfaces, which is adaptable to several research topics. The method provides a consistent quality of results. This also includes achieving reliable and comparable results and reducing the time and effort of conducting such studies. A standardized analysis method is provided by automated analysis tools that focus on statistical parameters. Specific key parameters and boundary conditions are defined for the tool application. The analysis relies on a database in which all key parameters are stored. These databases can be easily updated and adapted to various research questions. This increases the flexibility, reproducibility, and comparability of the research. However, the quality of the database and reliability of definitions directly influence the results. To ensure a high quality of results, the rules and definitions need to be well defined and based on previously conducted case studies. The tools then produce parameters, which are obtained by defined geostatistical techniques (measurements, calculations, classifications). The idea of an automated statistical analysis is tested to proof benefits but also potential problems of this method. In this study, I adapt automated tools for floor-fractured craters (FFCs) on Mars. These impact craters show a variety of surface features, occurring in different Martian environments, and having different fracturing origins. They provide a complex morphological and geological field of application. 433 FFCs are classified by the analysis tools due to their fracturing process. Spatial data, environmental context, and crater interior data are analyzed to distinguish between the processes involved in floor fracturing. Related geologic processes, such as glacial and fluvial activity, are too similar to be separately classified by the automated tools. Glacial and fluvial fracturing processes are merged together for the classification. The automated tools provide probability values for each origin model. To guarantee the quality and reliability of the results, classification tools need to achieve an origin probability above 50 %. This analysis method shows that 15 % of the FFCs are fractured by intrusive volcanism, 20 % by tectonic activity, and 43 % by water & ice related processes. In total, 75 % of the FFCs are classified to an origin type. This can be explained by a combination of origin models, superposition or erosion of key parameters, or an unknown fracturing model. Those features have to be manually analyzed in detail. Another possibility would be the improvement of key parameters and rules for the classification. This research shows that it is possible to conduct an automated statistical analysis of morphologic and geologic features based on analysis tools. Analysis tools provide additional information to the user and are therefore considered assistance systems.
Planetenforschung umfasst oft zeitintensive Projekte, bei denen Expertise und Erfahrung eine wesentliche Rolle spielen. Auf Grund äusserst komplexer und sich selten wiederholender Forschungsfragen sind Annahmen, Definitionen und Regeln zur Lösung dieser Fragen nicht leicht nachvollziehbar oder aber nicht eindeutig dokumentiert. Ein Vergleich der Ergebnisse unterschiedlicher Forscher zum selben Thema oder eine Erweiterung der Forschungsfrage macht dies somit nur schwer möglich. Vergleiche liefern oftmals verzerrte Ergebnisse, da die Ausgangslage und Randbedingungen unterschiedlich definiert worden sind. Das Ziel dieser Arbeit ist es eine Standardmethode zur Oberflächenanalyse zu entwickeln, die auf zahlreiche Untersuchungsfragen angewandt werden kann. Eine gleichbleibende Qualität der Ergebnisse muss durch diese Methode gewährleistet sein. Ein weiteres Ziel ist es, dass diese Methode ohne Vorwissen und Expertise angewandt werden kann und die Ergebnisse in kurzer Zeit vorliegen. Ausserdem müssen die Ergebnisse vergleichbar und nachvollziehbar sein. Automatisch operierende Analysewerkzeuge können die zahlreichen Anforderungen erfüllen und als Standardmethode dienen. Statistische Ergebnisse werden durch diese Methode erzielt. Die Werkzeuge basieren auf vordefinierten, geowissenschaftlichen Techniken und umfassen Messungen, Berechnungen und Klassifikationen der zu untersuchenden Oberflächenstrukturen. Für die Anwendung dieser Werkzeuge müssen Schlüsselstrukturen und Randbedingungen definiert werden. Des Weiteren benötigen die Werkzeuge eine Datenbank, in der alle Oberflächenstrukturen, aber auch Informationen zu den Randbedingungen gespeichert sind. Es ist mit geringem Aufwand möglich, Datenbanken zu aktualisieren und sie auf verschiedenste Fragestellungen zu adaptieren. Diese Tatsache steigert die Flexibilität, Reproduzierbarkeit und auch Vergleichbarkeit der Untersuchung. Die vordefinierten Randbedingungen und die Qualität der Datenbank haben jedoch auch direkten Einfluss auf die Qualität der Ergebnisse. Um eine gleichbleibend hohe Qualität der Untersuchung zu gewährleisten muss sichergestellt werden, dass alle vordefinierten Bedingungen eindeutig sind und auf vorheriger Forschung basieren. Die automatisch operierenden Analysewerkzeuge müssen als mögliche Standardmethode getestet werden. Hierbei geht es darum Vorteile, aber auch Nachteile zu identifizieren und zu bewerten. In dieser Arbeit werden die Analysewerkzeuge auf einen bestimmten Einschlagskratertyp auf dem Mars angewandt. Krater mit zerbrochenen Kraterböden (Floor-Fractured Craters) sind in verschiedensten Regionen auf dem Mars zu finden, sie zeigen zahlreiche Oberflächenstrukturen und wurden durch unterschiedliche Prozesse geformt. All diese Fakten machen diesen Kratertyp zu einem interessanten und im geologischen und morphologischen Sinne sehr komplexen Anwendungsgebiet. 433 Krater sind durch die Werkzeuge analysiert und je nach Entstehungsprozess klassifiziert worden. Für diese Analyse sind Position der Krater, Art des Umfeldes und Strukturen im Kraterinneren ausschlaggebend. Die kombinierten Informationen geben somit Auskunft über die Prozesse, welche zum Zerbrechen des Kraterbodens geführt haben. Die entwickelten Analysewerkzeuge können geologische Prozesse, die sehr ähnlich zueinander sind, von einander abhängig sind und zusätzlich auch dieselben Oberflächenstrukturen formen, nicht eindeutig unterscheiden. Aus diesem Grund sind fluviale und glaziale Entstehungsprozesse für den untersuchten Kratertyp zusammengefasst. Die Analysewerkzeuge liefern Wahrscheinlichkeitswerte für drei mögliche Entstehungsarten. Um die Qualität der Ergebnisse zu verbessern muss eine Wahrscheinlichkeit über 50 % erreicht werden. Die Werkzeuge zeigen, dass 15 % der Krater durch Vulkanismus, 20 % durch Tektonik und 43 % durch Wasser- und Eis-bedingte Prozesse gebildet wurden. Insgesamt kann für 75 % des untersuchten Kratertyps ein potentieller Entstehungsprozess zugeordnet werden. Für 25 % der Krater ist eine Klassifizierung nicht möglich. Dies kann durch eine Kombination von geologischen Prozessen, einer Überprägung von wichtigen Schlüsselstrukturen, oder eines bisher nicht berücksichtigten Prozesses erklärt werden. Zusammenfassend ist zu sagen, dass es möglich ist planetare Oberflächenstrukturen quantitativ durch automatisch operierende Analysewerkzeuge zu erfassen und hinsichtlich einer definierten Fragestellung zu klassifizieren. Zusätzliche Informationen können durch die entwickelten Werkzeuge erhalten werden, daher sind sie als Assistenzsystem zu betrachten.

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Perälä, Jesper. "Pit Craters of Arsia Mons Volcano, Mars, and Their Relation to Regional Volcano-tectonism." Thesis, Uppsala universitet, Institutionen för geovetenskaper, 2015. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-255563.

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Pit crater and pit crater chains associated to the volcano Arsia Mons on Mars have been mapped to analyse their spatial pattern and to conclude about their formation. For the mapping, high resolution satellite data gathered during the Mars Express mission were used. The spatial distribution of the pit craters was then compared with typical patterns of magmatic sheet intrusions within volcanoes as they are known from Earth. The results show that the pattern of the mapped pit craters and pit crater chains are in good agreement with these sheet intrusions and are therefore likely related to Martian sheet intrusions.
Kollapskratrar och kraterkedjor relaterade till vulkanen Arsia Mons på Mars har karterats för att analysera deras spatiala mönster och för att komma till slutsatser för deras tillblivelse. Högupplösta satellitbilder tagna av Mars Express-sonden har använts för karteringen. Fördelningen av de karterade kraterkedjorna jämfördes med typiska fördelningar av magmatiska gångbergarter från vulkaner på jorden. Resultaten visar att fördelningen av kollapskratrar och kraterkedjor överensstämmer enligt förväntningarna och påvisar en relation mellan kollapskratrar och magmatiska gångbergarter på Mars.

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Viola, Donna, and Donna Viola. "Expanded Craters on Mars: Implications for Shallow, Mid-Latitude Excess Ice." Diss., The University of Arizona, 2017. http://hdl.handle.net/10150/625594.

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Understanding the age and distribution of shallow ice on Mars is valuable for interpreting past and present climate conditions, and has implications on habitability and future in situ resource utilization. Many ice-related features, such as lobate debris aprons and concentric crater fill, have been studied using a range of remote sensing techniques. Here, I explore the distribution of expanded craters, a form of sublimation thermokarst where shallow, excess ice has been destabilized and sublimated following an impact event. This leads to the collapse of the overlying dry regolith to produce the appearance of diameter widening. The modern presence of these features suggests that excess ice has remained preserved in the terrain immediately surrounding the craters since the time of their formation in order to maintain the surface. High-resolution imagery is ideal for observing thermokarst features, and much of the work described here will utilize data from the Context Camera (CTX) and High Resolution Imaging Science Experiment (HiRISE) on the Mars Reconnaissance Orbiter (MRO). Expanded craters tend to be found in clusters that emanate radially from at least four primary craters in Arcadia Planitia, and are interpreted as secondary craters that formed nearly simultaneously with their primaries. Crater age dates of the primaries indicate that the expanded secondaries, as well as the ice layer into which they impacted, must be at least tens of millions of years old. Older double-layer ejecta craters in Arcadia Planitia commonly have expanded craters superposed on their ejecta – and they tend to be more expanded (with larger diameters) in the inner ejecta layer. This has implications on the formation mechanisms for craters with this unique ejecta morphology. Finally, I explore the distribution of expanded craters south of Arcadia Planitia and across the southern mid-latitudes, along with scalloped depressions (another form of sublimation thermokarst), in order to identify the modern excess ice boundary in this region and any longitudinal variations. This study identifies some potential low-latitude locations with patchy excess ice, possibly preserved during a past climate. Through these studies, I will infer regions that contain abundant ice today and consider the implications that this ice has on both the martian climate and future exploration.

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Breton, Sylvain. "Dynamique des surfaces planétaires actives : quantification des paysages, modélisation et inversion." Thesis, Lyon, 2019. http://www.theses.fr/2019LYSE1280.

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Les cratères d'impact sont indispensables dans l'étude des surfaces planétaires. D'une part, les statistiques de leur nombre permet de dater les surfaces planétaires, d'autre part, leur forme révèle les processus de surface qu'ils ont connu. Cette thèse propose de coupler les études statistiques et morphologiques afin d'étudier la temporalité et l'importance des processus sédimentaires et/ou volcaniques des surfaces planétaires. L'utilisation de la profondeur des cratères permet de rajouter une dimension aux distributions avec l'introduction des distributions en fréquence de taille et de profondeur (SDFD), offrant ainsi un aperçu des modifications morphologiques des cratères. Nous avons développé en conséquence des modèles permettant de modéliser l'évolution d'une population de cratères en prenant en compte les phénomènes d'oblitération. La surface Mars est largement cratérisée, mais ils ont pour la plupart été fortement modifiés par des processus volcaniques et/ou sédimentaires. A partir des SDFDs, nous avons estimé les taux d'oblitération martiens à une échelle globale. Ces taux sont, au Noachien, de plusieurs milliers de m/Ga, mais décroissent rapidement dès l'Hespérien inférieur et sont proches de 0 à l'Amazonien. L'oblitération sur la province de Tharsis a décru beaucoup moins rapidement suggérant une persistance du volcanisme à l'Amazonien inférieur. Les plaines du nord à l'Amazonien sont marqué par des taux d'oblitération un ordre de grandeur au-dessus du reste de la planète, qui pourraient indiquer la mise en place continue de la Vastitas Borealis Formation au cours de l'Amazonien moyen. En complément de notre approche à l'échelle globale, nous avons déterminé des taux d'oblitération actuels à partir de cartographies de cratères réalisées à haute résolution spatiale sur des sites d'atterrissage de rovers actuels et futurs. Les sites de Mawrth Vallis et d'Oxia Planum présentent les taux d'oblitération actuels les plus importants en particulier au niveau de leurs unités geologiques riches en minéraux hydratés
Impact crater are often used in the study of planetary surfaces. On the one hand, statistics on crater number provide the age of the surface, on the other hand, their shapes reflect the surface processes they witnessed. This study combines the statistic and morphology approaches in order to investigate the timing and intensity of sedimentary and volcanic processes of planetary surfaces. The use of crater depth measurements add a dimension to frequency distributions with the introduction of size and depth frequency distribution (SDFD). SDFSs can be interpreted in term of crater obliteration rates thanks to crater chronology models. We also developed models of crater population taking into account obliteration. Mars surface is highly cratered with many craters displaying signs of modifications by volcanic process, sedimentation and erosion. We interpreted SDFDs using a classic crater chronology system, to produce global maps of obliteration at different epochs of Mars. During Noachian, obliteration rates reach several thousands m/Gy, but rapidly decrease during early Hesperian and are close to 0 during Amazonian. Obliteration on the province of Tharsis decreased slower, suggesting a persistence of volcanic activity until early Amazonian. Northern lowlands witness Amazonian obliteration rates one order of magnitude higher than the rest of the planet, which may indicate the continuous formation of Vastitas Borealis during middle Amazonian. In addition to our global approach, we computed recent obliteration rates from mapping of high resolution images on landing sites of rover missions. Mawrth Vallis and Oxia Planum present significant obliteration rates, especially on units containing hydrated minerals

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Viola, D., and A. S. McEwen. "Geomorphological Evidence for Shallow Ice in the Southern Hemisphere of Mars." AMER GEOPHYSICAL UNION, 2018. http://hdl.handle.net/10150/627126.

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The localized loss of near-surface excess ice on Mars by sublimation (and perhaps melting) can produce thermokarstic collapse features such as expanded craters and scalloped depressions, which can be indicators of the preservation of shallow ice. We demonstrate this by identifying High Resolution Imaging Science Experiment images containing expanded craters south of Arcadia Planitia (25-40 degrees N) and observe a spatial correlation between regions with thermokarst and the lowest-latitude ice-exposing impact craters identified to date. In addition to widespread thermokarst north of 35 degrees N, we observe localized thermokarst features that we interpret as patchy ice as far south as 25 degrees N. Few ice-exposing craters have been identified in the southern hemisphere of Mars since they are easier to find in dusty, high-albedo regions, but the relationship among expanded craters, ice-exposing impacts, and the predicted ice table boundary in Arcadia Planitia allows us to extend this thermokarst survey into the southern midlatitudes (30-60 degrees S) to infer the presence of ice today. Our observations suggest that the southern hemisphere excess ice boundary lies at 45 degrees S regionally. At lower latitudes, some isolated terrains (e.g., crater fill and pole-facing slopes) also contain thermokarst, suggesting local ice preservation. We look for spatial relationships between our results and surface properties (e.g., slope and neutron spectrometer water ice concentration) and ice table models to understand the observed ice distribution. Our results show trends with thermal inertia and dust cover and are broadly consistent with ice deposition during a period with a higher relative humidity than today. Shallow, lower-latitude ice deposits are of interest for future exploration.

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Books on the topic "Mars craters"

1

Grant, John A. Advances in planetary geology. Washington: NASA, 1987.

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Bridges, John C. Evolution of the Martian Crust. Oxford University Press, 2017. http://dx.doi.org/10.1093/acrefore/9780190647926.013.18.

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This is an advance summary of a forthcoming article in the Oxford Encyclopedia of Planetary Science. Please check back later for the full article.Mars, which has a tenth of the mass of Earth, has cooled as a single lithospheric plate. Current topography gravity maps and magnetic maps do not show signs of the plate tectonics processes that have shaped the Earth’s surface. Instead, Mars has been shaped by the effects of meteorite bombardment, igneous activity, and sedimentary—including aqueous—processes. Mars also contains enormous igneous centers—Tharsis and Elysium, with other shield volcanoes in the ancient highlands. In fact, the planet has been volcanically active for nearly all of its 4.5 Gyr history, and crater counts in the Northern Lowlands suggest that may have extended to within the last tens of millions of years. Our knowledge of the composition of the igneous rocks on Mars is informed by over 100 Martian meteorites and the results from landers and orbiters. These show dominantly tholeiitic basaltic compositions derived by melting of a relatively K, Fe-rich mantle compared to that of the Earth. However, recent meteorite and lander results reveal considerable diversity, including more silica-rich and alkaline igneous activity. These show the importance of a range of processes including crystal fractionation, partial melting, and possibly mantle metasomatism and crustal contamination of magmas. The figures and plots of compositional data from meteorites and landers show the range of compositions with comparisons to other planetary basalts (Earth, Moon, Venus). A notable feature of Martian igneous rocks is the apparent absence of amphibole. This is one of the clues that the Martian mantle had a very low water content when compared to that of Earth.The Martian crust, however, has undergone hydrothermal alteration, with impact as an important heat source. This is shown by SNC analyses of secondary minerals and Near Infra-Red analyses from orbit. The associated water may be endogenous.Our view of the Martian crust has changed since Viking landers touched down on the planet in 1976: from one almost entirely dominated by basaltic flows to one where much of the ancient highlands, particularly in ancient craters, is covered by km deep sedimentary deposits that record changing environmental conditions from ancient to recent Mars. The composition of these sediments—including, notably, the MSL Curiosity Rover results—reveal an ancient Mars where physical weathering of basaltic and fractionated igneous source material has dominated over extensive chemical weathering.

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Reimold, Wolf Uwe, and Christian Koeberl, eds. Large Meteorite Impacts and Planetary Evolution VI. Geological Society of America, 2021. http://dx.doi.org/10.1130/spe550.

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This volume represents the proceedings of the homonymous international conference on all aspects of impact cratering and planetary science, which was held in October 2019 in Brasília, Brazil. This volume contains a sizable suite of contributions dealing with regional impact records (Australia, Sweden), impact craters and impactites, early Archean impacts and geophysical characteristics of impact structures, shock metamorphic investigations, post-impact hydrothermalism, and structural geology and morphometry of impact structures—on Earth and Mars. These contributions are authored by many of the foremost impact cratering researchers. Many contributions report results from state-of-the-art investigations, for example, several that are based on electron backscatter diffraction studies, and deal with new potential chronometers and shock barometers (e.g., apatite). Established impact cratering workers and newcomers to this field will both appreciate this multifaceted, multidisciplinary collection of impact cratering studies.

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E, Wieprecht David, and Sako Maurice K, eds. Elevations and descriptions for leveling bench marks at Newberry Crater, Oregon. [Reston, Va.]: U.S. Dept. of the Interior, U.S. Geological Survey, 1995.

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Byrne, Charles J. The Moon's Largest Craters and Basins: Images and Topographic Maps from LRO, GRAIL, and Kaguya. Springer, 2016.

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Byrne, Charles J. The Moon's Largest Craters and Basins: Images and Topographic Maps from LRO, GRAIL, and Kaguya. Springer, 2015.

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Survey, United States Geological. Geologic map of the MTM -15182 and MTM -15187 quadrangles, Gusev Crater-Ma'adim Vallis Region, Mars. For sale by USGS Information Services, 2000.

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Washington, Oregon: Includes Maps of Portland, Seattle, Crater Lake NP, Mount Rainier NP. Not Avail, 2004.

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Cogenetic rock fragments from a lunar soil: Evidence of a ferroan noritic-anorthosite pluton on the moon. [Washington, DC: National Aeronautics and Space Administration, 1995.

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Verne, Jules. Journey to the Centre of the Earth. Translated by William Butcher. Oxford University Press, 2008. http://dx.doi.org/10.1093/owc/9780199538072.001.0001.

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Journey to the Centre of the Earth has been consistently praised for its style and its vision of the world. It explores the prehistory of the globe, but can also be read as a psychological quest, for the journey itself is as important as arrival or discovery. Professor Lidenbrock and his nephew Axel travel across Iceland, and then down through an extinct crater towards a sunless sea where they enter a living past and are confronted with the origins of man. A classic of nineteenth-century French literature, the novel's distinctive combination of realism and Romanticism has marked figures as diverse as Sartre and Tournier, Mark Twain and Conan Doyle. This new translation of the complete text is faithful to the lyricism, verve, and humour of the original.

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Book chapters on the topic "Mars craters"

1

Vetro, Rosanne, and Dan A. Simovici. "Entropic Quadtrees and Mining Mars Craters." In Advances in Data Mining. Applications and Theoretical Aspects, 210–21. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-14400-4_17.

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Chapman, Clark R., and David Morrison. "Craters on the Moon and Mars." In Cosmic Catastrophes, 41–58. Boston, MA: Springer US, 1989. http://dx.doi.org/10.1007/978-1-4899-6553-0_4.

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Barata, Teresa, E. Ivo Alves, José Saraiva, and Pedro Pina. "Automatic Recognition of Impact Craters on the Surface of Mars." In Lecture Notes in Computer Science, 489–96. Berlin, Heidelberg: Springer Berlin Heidelberg, 2004. http://dx.doi.org/10.1007/978-3-540-30126-4_60.

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Marques, Jorge S., and Pedro Pina. "An Algorithm for the Delineation of Craters in Very High Resolution Images of Mars Surface." In Pattern Recognition and Image Analysis, 213–20. Berlin, Heidelberg: Springer Berlin Heidelberg, 2013. http://dx.doi.org/10.1007/978-3-642-38628-2_25.

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Hargitai, Henrik. "Pedestal Crater (Mars)." In Encyclopedia of Planetary Landforms, 1–8. New York, NY: Springer New York, 2014. http://dx.doi.org/10.1007/978-1-4614-9213-9_257-1.

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Hargitai, Henrik. "Pedestal Crater (Mars)." In Encyclopedia of Planetary Landforms, 1535–41. New York, NY: Springer New York, 2015. http://dx.doi.org/10.1007/978-1-4614-3134-3_257.

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Airo, Alessandro. "Crater Lakes (Mars)." In Encyclopedia of Astrobiology, 1. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-27833-4_3244-2.

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Airo, Alessandro. "Crater Lakes (Mars)." In Encyclopedia of Astrobiology, 582. Berlin, Heidelberg: Springer Berlin Heidelberg, 2015. http://dx.doi.org/10.1007/978-3-662-44185-5_3244.

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Cattermole, Peter. "The Ancient Cratered Terrain." In Mars, 52–70. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2306-8_6.

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El-Maarry, Mohamed Ramy, Richard Soare, and Ákos Kereszturi. "Crater-Floor Polygons (Mars)." In Encyclopedia of Planetary Landforms, 1–6. New York, NY: Springer New York, 2014. http://dx.doi.org/10.1007/978-1-4614-9213-9_72-2.

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Conference papers on the topic "Mars craters"

1

Schultz, Peter H. "MISSING MARS: CLUES FROM RELICT CRATERS." In GSA Annual Meeting in Seattle, Washington, USA - 2017. Geological Society of America, 2017. http://dx.doi.org/10.1130/abs/2017am-306336.

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Wilson, Sharon A., and Alan D. Howard. "THE NATURE AND DISTRIBUTION OF POLLYWOG CRATERS ON MARS." In GSA Annual Meeting in Phoenix, Arizona, USA - 2019. Geological Society of America, 2019. http://dx.doi.org/10.1130/abs/2019am-339375.

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Kling, Corbin L., Paul K. Byrne, Danielle Y. Wyrick, Karl W. Wegmann, and Helena Mitasova. "THE FORMATION OF PIT CRATERS WITHIN NOCTIS LABYRINTHUS, MARS." In GSA Annual Meeting in Seattle, Washington, USA - 2017. Geological Society of America, 2017. http://dx.doi.org/10.1130/abs/2017am-307391.

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Golombek, M. P., N. H. Warner, Vamsi Ganti, and Julianne Sweeney. "DEGRADATION OF SMALL IMPACT CRATERS: EROSION RATES AND MARS CLIMATE." In GSA Annual Meeting in Seattle, Washington, USA - 2017. Geological Society of America, 2017. http://dx.doi.org/10.1130/abs/2017am-301049.

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Aoki, Risako, Akira Oyama, Koji Fujita, Hiroki Nagai, Masahiro Kanazaki, Kensuke Kanou, Nao Inoue, Shu Sokabe, Kai Tomisawa, and Kazufumi Uwatoko. "Conceptual Helicopter Design for Exploration of Pit craters and Caves on Mars." In 2018 AIAA SPACE and Astronautics Forum and Exposition. Reston, Virginia: American Institute of Aeronautics and Astronautics, 2018. http://dx.doi.org/10.2514/6.2018-5362.

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Wilson, Sharon A., Alexander M. Morgan, and Alan D. Howard. "THE GLOBAL DISTRIBUTION OF CRATERS WITH ALLUVIAL FANS AND DELTAS ON MARS." In GSA 2020 Connects Online. Geological Society of America, 2020. http://dx.doi.org/10.1130/abs/2020am-359423.

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Newsom, Horton E. "Where Should We Look for Life on Mars: The Case for Impact Craters?" In SPACE TECHNOLOGY AND APPLICATIONS INTERNAT.FORUM-STAIF 2004: Conf.on Thermophys.in Microgravity; Commercial/Civil Next Gen.Space Transp.; 21st Symp.Space Nuclear Power & Propulsion; Human Space Explor.; Space Colonization; New Frontiers & Future Concepts. AIP, 2004. http://dx.doi.org/10.1063/1.1649658.

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Irwin, Rossman, and Edward Wolfe. "SPATIALLY AND TEMPORALLY VARIABLE EROSION OF THE LARGEST POST-NOACHIAN IMPACT CRATERS ON MARS." In GSA 2020 Connects Online. Geological Society of America, 2020. http://dx.doi.org/10.1130/abs/2020am-358202.

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Peel, Samantha E., and Devon M. Burr. "MAPPING LACUSTRINE, FLUVIAL, AND AEOLIAN DEPOSITS WITHIN CRATERS IN THE AEOLIS DORSA REGION OF MARS." In 67th Annual Southeastern GSA Section Meeting - 2018. Geological Society of America, 2018. http://dx.doi.org/10.1130/abs/2018se-312598.

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Harrison, Tanya N. "EVIDENCE FOR VOLCANISM IN MARTIAN FLOOR-FRACTURED CRATERS FROM THE MARS RECONNAISSANCE ORBITER CONTEXT CAMERA." In GSA Annual Meeting in Seattle, Washington, USA - 2017. Geological Society of America, 2017. http://dx.doi.org/10.1130/abs/2017am-308639.

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Reports on the topic "Mars craters"

1

Joseph, Rhawn. Mars: Algae, Lichens, Fossils, Minerals, Microbial Mats, and Stromatolites in Gale Crater. Journal of Astrobiology and Space Science, March 2020. http://dx.doi.org/10.37720/jassr.03082020.

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Berger, B., D. Blaney, J. Bridges, A. Cousin, O. Forni, O. Gasnault, J. Lasue, et al. POSSIBLE ALTERATION OF ROCKS OBSERVED BY CHEMCAM ALONG THE TRAVERSE TO GLENELG IN GALE CRATER ON MARS. Office of Scientific and Technical Information (OSTI), April 2013. http://dx.doi.org/10.2172/1077020.

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Geologic map of the MTM-15182 and MTM-15187 quadrangles, Gusev Crater-Ma'adim Vallis region, Mars. US Geological Survey, 2000. http://dx.doi.org/10.3133/i2666.

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Maps showing posteruption erosion, deposition, and dome growth in Mount St. Helens Crater, Washington, determined by a geographic information system. US Geological Survey, 1992. http://dx.doi.org/10.3133/i2297.

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