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Journal articles on the topic 'Mars craters'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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1

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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2

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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3

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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4

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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5

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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6

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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7

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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8

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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9

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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10

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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11

Anderer, Michael. "John Mellish and the Craters of Mars." Highlights of Astronomy 10 (1995): 133–34. http://dx.doi.org/10.1017/s1539299600010625.

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12

Berman, Daniel C., David A. Crown, and Leslie F. Bleamaster. "Degradation of mid-latitude craters on Mars." Icarus 200, no. 1 (March 2009): 77–95. http://dx.doi.org/10.1016/j.icarus.2008.10.026.

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13

Stepinski, Tomasz F., Michael P. Mendenhall, and Brian D. Bue. "Machine cataloging of impact craters on Mars." Icarus 203, no. 1 (September 2009): 77–87. http://dx.doi.org/10.1016/j.icarus.2009.04.026.

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14

Brolly, Connor, John Parnell, and Stephen Bowden. "Raman spectroscopy of shocked gypsum from a meteorite impact crater." International Journal of Astrobiology 16, no. 3 (September 21, 2016): 286–92. http://dx.doi.org/10.1017/s1473550416000367.

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AbstractImpact craters and associated hydrothermal systems are regarded as sites within which life could originate on Earth, and on Mars. The Haughton impact crater, one of the most well preserved craters on Earth, is abundant in Ca-sulphates. Selenite, a transparent form of gypsum, has been colonized by viable cyanobacteria. Basement rocks, which have been shocked, are more abundant in endolithic organisms, when compared with un-shocked basement. We infer that selenitic and shocked gypsum are more suitable for microbial colonization and have enhanced habitability. This is analogous to many Martian craters, such as Gale Crater, which has sulphate deposits in a central layered mound, thought to be formed by post-impact hydrothermal springs. In preparation for the 2020 ExoMars mission, experiments were conducted to determine whether Raman spectroscopy can distinguish between gypsum with different degrees of habitability. Ca-sulphates were analysed using Raman spectroscopy and results show no significant statistical difference between gypsum that has experienced shock by meteorite impact and gypsum, which has been dissolved and re-precipitated as an evaporitic crust. Raman spectroscopy is able to distinguish between selenite and unaltered gypsum. This shows that Raman spectroscopy can identify more habitable forms of gypsum, and demonstrates the current capabilities of Raman spectroscopy for the interpretation of gypsum habitability.

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15

Nikora, Vladimir, and Derek Goring. "Spectral scaling in Mars topography: effect of craters." Acta Geophysica 54, no. 1 (March 2006): 102–12. http://dx.doi.org/10.2478/s11600-006-0009-8.

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16

Bamberg, M., R. Jaumann, H. Asche, T. Kneissl, and G. G. Michael. "Floor-Fractured Craters on Mars – Observations and Origin." Planetary and Space Science 98 (August 2014): 146–62. http://dx.doi.org/10.1016/j.pss.2013.09.017.

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17

Ormö, Jens, James M. Dohm, Justin C. Ferris, Alain Lepinette, and Alberto G. Fairén. "Marine-target craters on Mars? An assessment study." Meteoritics & Planetary Science 39, no. 2 (February 2004): 333–46. http://dx.doi.org/10.1111/j.1945-5100.2004.tb00344.x.

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18

Crumpler, L. S., R. E. Arvidson, D. W. Mittlefehldt, J. A. Grant, and W. H. Farrand. "Results from the first geologic traverse on the topographic rim of a complex impact crater, Endeavour Crater, Mars." Geology 48, no. 3 (December 17, 2019): 252–57. http://dx.doi.org/10.1130/g46903.1.

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Abstract A geologic traverse along the rim of the 22-km-diameter Endeavour Crater by the Opportunity Mars rover has provided the first field geologic observations of outcrop-scale structure and stratigraphy at a complex impact crater, characteristics that were previously undocumented due to erosion of similar-size craters on Earth. Two findings of note are (1) the attitude of sheets, foliations, and contacts between rim impact breccias and pre-impact substrate is antiformal, the limbs dipping inward toward the center of the crater inside the crater rim and outward exterior to the crater rim; and (2) coherent blocks of crust segment the rim topographically and structurally into a series of right- and left-stepping elongate rises of variable size and orientation. These segments experienced differing magnitudes of uplift during crater formation along identified vertical scissors faults. Brecciation along the faults bounding rim segments created zones of enhanced subsurface fluid transport through the crater rim, potentially responsible for localized areas of aqueous alteration identified in outcrops near segment boundaries.

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19

Day, Mackenzie D., and David C. Catling. "Potential aeolian deposition of intra-crater layering: A case study of Henry crater, Mars." GSA Bulletin 132, no. 3-4 (June 6, 2019): 608–16. http://dx.doi.org/10.1130/b35230.1.

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Abstract Layered deposits occur on Mars in a wide variety of settings and morphologies, including inside craters as large mounds. Many origins have been proposed for these intra-crater layered deposits, but recent work has suggested the possibility of deposition by ancient aeolian dunes. Distinguishing dune deposits requires identifying cross-strata which may not be resolvable even with the highest spatial resolution imaging of Mars. In this work, we employ an alternative method and attempt to eliminate the possibility of aeolian deposition by comparing martian layer geometries to the angles and thicknesses of aeolian sets on Earth. Layering in Henry crater falls within the expected bounds for aeolian strata, and if ancient dunes deposited these layers, then the sets record the passage of dunes with 10–100 m spacing that were generally migrating toward the center of the crater. The Henry crater mound comprises ∼8000 km3 of sediment, and if all layers reflect dune deposition, we estimate mound deposition would then take at least ∼0.5 m.y. As a whole, ∼20,000 km3 of sediment are preserved in intra-crater layered deposits in Arabia Terra. Results from this case study of Henry crater suggest that at least some of this volume may be from aeolian dunes, in which case intra-crater layered mounds may host an untapped record of very ancient martian aeolian activity.

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20

Ksanfomality, L. V. "Paradox of Flows on Mars." Highlights of Astronomy 13 (2005): 918–20. http://dx.doi.org/10.1017/s1539299600017597.

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Using the high-resolution images acquired by cameras onboard the MARS GLOBAL SURVEYOR orbiter made it possible to reveal the previously unknown objects on the Martian surface, which changed dramatically a notion of Mars as a dry, hydrologically dead planet (Malin and Edgett, 2000). Examination of new images shows that the nature of some extended dark formations on the slopes of craters and uplands may be associated with contemporary abundant sources of liquid water arising on the slopes at small depths below the level of surrounding plains.

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21

Schmitt, Harrison H. "Life among the Craters." Symposium - International Astronomical Union 213 (2004): 199–202. http://dx.doi.org/10.1017/s0074180900193271.

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The Moon forms one end-member in the planetary mass series Earth-Venus-Mars-Mercury-Asteroids-Moon (Weissman 1999). Having a detailed understanding of the nature and evolution of the two end-members of this series, rather than of just the Earth, has increased the value of other data and inferences by orders of magnitude. As a consequence of obtaining an understanding of the evolution of a second planet, we now can look at other terrestrial planets with far greater insight than ever would have been possible otherwise (Fig. 1).

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22

Shean, David E. "Candidate ice-rich material within equatorial craters on Mars." Geophysical Research Letters 37, no. 24 (December 2010): n/a. http://dx.doi.org/10.1029/2010gl045181.

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23

Morris, Aisha R., and Peter J. Mouginis-Mark. "Thermally distinct craters near Hrad Vallis, Elysium Planitia, Mars." Icarus 180, no. 2 (February 2006): 335–47. http://dx.doi.org/10.1016/j.icarus.2005.09.015.

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24

Wadhwa, Surjit S. "Data analysis of craters, calderas and shadows on Mars." Physics Education 37, no. 4 (July 1, 2002): 342–43. http://dx.doi.org/10.1088/0031-9120/37/4/404.

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25

Barlow, N. G. "What we know about Mars from its impact craters." Geological Society of America Bulletin 122, no. 5-6 (December 30, 2009): 644–57. http://dx.doi.org/10.1130/b30182.1.

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26

Robbins, Stuart J., and Brian M. Hynek. "Distant secondary craters from Lyot crater, Mars, and implications for surface ages of planetary bodies." Geophysical Research Letters 38, no. 5 (March 2, 2011): n/a. http://dx.doi.org/10.1029/2010gl046450.

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27

Schwenzer, S. P., O. Abramov, C. C. Allen, S. M. Clifford, C. S. Cockell, J. Filiberto, D. A. Kring, et al. "Puncturing Mars: How impact craters interact with the Martian cryosphere." Earth and Planetary Science Letters 335-336 (June 2012): 9–17. http://dx.doi.org/10.1016/j.epsl.2012.04.031.

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28

Kuzmin, R. "Wind-Related Modification of Some Small Impact Craters on Mars." Icarus 153, no. 1 (September 2001): 61–70. http://dx.doi.org/10.1006/icar.2001.6654.

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29

Fairen, A. G., V. Chevrier, O. Abramov, G. A. Marzo, P. Gavin, A. F. Davila, L. L. Tornabene, et al. "Noachian and more recent phyllosilicates in impact craters on Mars." Proceedings of the National Academy of Sciences 107, no. 27 (July 6, 2010): 12095–100. http://dx.doi.org/10.1073/pnas.1002889107.

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30

Schmerr, N. C., M. E. Banks, and I. J. Daubar. "The Seismic Signatures of Recently Formed Impact Craters on Mars." Journal of Geophysical Research: Planets 124, no. 11 (November 2019): 3063–81. http://dx.doi.org/10.1029/2019je006044.

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31

Mouginis-Mark, Peter J., and Joan N. Hayashi. "Shallow and deep fresh impact craters in Hesperia Planum, Mars." Earth, Moon, and Planets 61, no. 1 (April 1993): 1–20. http://dx.doi.org/10.1007/bf00619135.

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32

Jankowski, David G., and Steven W. Squyres. "The topography of impact craters in “softened” terrain on Mars." Icarus 100, no. 1 (November 1992): 26–39. http://dx.doi.org/10.1016/0019-1035(92)90015-y.

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33

Liu, Jia, Zongyu Yue, Kaichang Di, Sheng Gou, and Shengli Niu. "A Study about the Temporal Constraints on the Martian Yardangs’ Development in Medusae Fossae Formation." Remote Sensing 13, no. 7 (March 30, 2021): 1316. http://dx.doi.org/10.3390/rs13071316.

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The age of Mars yardangs is significant in studying their development and the evolution of paleoclimate conditions. For planetary surface or landforms, a common method for dating is based on the frequency and size distribution of all the superposed craters after they are formed. However, there is usually a long duration for the yardangs’ formation, and they will alter the superposed craters, making it impossible to give a reliable dating result with the method. An indirect method by analyzing the ages of the superposed layered ejecta was devised in the research. First, the layered ejecta that are superposed on and not altered by the yardangs are identified and mapped. Then, the ages of the layered ejecta are derived according to the crater frequency and size distribution on them. These ages indicate that the yardangs ceased development by these times, and the ages are valuable for studying the evolution of the yardangs. This indirect dating method was applied to the areas of Martian yardangs in the Medusae Fossae Formation (MFF). The ages of the selected six layered ejecta range from ~0.50 Ga to ~1.5 Ga, indicating that the evolution of the corresponding yardangs had been ceased before these times. Analysis of more layered ejecta craters and superposed yardangs implies that yardangs in the MFF have a long history of development and some yardangs are still in active development.

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34

Kadish, Seth J., and James W. Head. "Impacts into non-polar ice-rich paleodeposits on Mars: Excess ejecta craters, perched craters and pedestal craters as clues to Amazonian climate history." Icarus 215, no. 1 (September 2011): 34–46. http://dx.doi.org/10.1016/j.icarus.2011.07.014.

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35

Hirase, Yoshiaki, Akiko M. Nakamura, and Tatsuhiro Michikami. "Ejecta size-velocity relation derived from the distribution of the secondary craters of kilometer-sized craters on Mars." Planetary and Space Science 52, no. 12 (October 2004): 1103–8. http://dx.doi.org/10.1016/j.pss.2004.07.007.

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36

Caprarelli, Graziella, and Roberto Orosei. "Probing the Hidden Geology of Isidis Planitia (Mars) with Impact Craters." Geosciences 5, no. 1 (February 13, 2015): 30–44. http://dx.doi.org/10.3390/geosciences5010030.

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37

Baioni, Davide, and Mario Tramontana. "Possible karst landforms in two unnamed craters in Tyrrhena Terra, Mars." Planetary and Space Science 132 (November 2016): 57–65. http://dx.doi.org/10.1016/j.pss.2016.08.011.

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38

Barlow, Nadine G. "The degradation of impact craters in Maja Valles and Arabia, Mars." Journal of Geophysical Research 100, E11 (1995): 23307. http://dx.doi.org/10.1029/95je02492.

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39

Daubar, Ingrid J., C. Atwood-Stone, S. Byrne, A. S. McEwen, and P. S. Russell. "The morphology of small fresh craters on Mars and the Moon." Journal of Geophysical Research: Planets 119, no. 12 (December 2014): 2620–39. http://dx.doi.org/10.1002/2014je004671.

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40

Kadish, Seth J., and James W. Head. "Preservation of layered paleodeposits in high-latitude pedestal craters on Mars." Icarus 213, no. 2 (June 2011): 443–50. http://dx.doi.org/10.1016/j.icarus.2011.03.029.

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41

Turner, Stuart M. R., John C. Bridges, Stephen Grebby, and Bethany L. Ehlmann. "Hydrothermal activity recorded in post Noachian-aged impact craters on Mars." Journal of Geophysical Research: Planets 121, no. 4 (April 2016): 608–25. http://dx.doi.org/10.1002/2015je004989.

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42

Peel, Samantha E., and Caleb I. Fassett. "Valleys in pit craters on Mars: Characteristics, distribution, and formation mechanisms." Icarus 225, no. 1 (July 2013): 272–82. http://dx.doi.org/10.1016/j.icarus.2013.03.031.

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43

Williams, Jean-Pierre, Asmin V. Pathare, and Oded Aharonson. "The production of small primary craters on Mars and the Moon." Icarus 235 (June 2014): 23–36. http://dx.doi.org/10.1016/j.icarus.2014.03.011.

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Williams, Nathan R., James F. Bell, Philip R. Christensen, and Jack D. Farmer. "Evidence for an explosive origin of central pit craters on Mars." Icarus 252 (May 2015): 175–85. http://dx.doi.org/10.1016/j.icarus.2014.12.005.

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OBERBECK, Verne R. "Layered ejecta craters and the early water/ice aquifer on Mars." Meteoritics & Planetary Science 44, no. 1 (January 2009): 43–54. http://dx.doi.org/10.1111/j.1945-5100.2009.tb00716.x.

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Li, L., Z. Yue, C. Zhang, and D. Li. "REMOTE SENSING OBSERVATIONS AND NUMERICAL SIMULATION FOR MARTIAN LAYERED EJECTA CRATERS." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XLII-3 (April 30, 2018): 865–70. http://dx.doi.org/10.5194/isprs-archives-xlii-3-865-2018.

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Abstract:

To understand past Martian climates, it is important to know the distribution and nature of water ice on Mars. Impact craters are widely used ubiquitous indicators for the presence of subsurface water or ice on Mars. Remote sensing observations and numerical simulation are powerful tools for investigating morphological and topographic features on planetary surfaces, and we can use the morphology of layered ejecta craters and hydrocode modeling to constrain possible layering and impact environments. The approach of this work consists of three stages：Firstly, the morphological characteristics of the Martian layered ejecta craters are performed based on Martian images and DEM data. Secondly, numerical modeling layered ejecta are performed through the hydrocode iSALE (impact-SALE). We present hydrocode modeling of impacts onto targets with a single icy layer within an otherwise uniform basalt crust to quantify the effects of subsurface H<sub>2</sub>O on observable layered ejecta morphologies. The model setup is based on a layered target made up of a regolithic layer (described by the basalt ANEOS), on top an ice layer (described by ANEOS equation of H<sub>2</sub>O ice), in turn on top of an underlying basaltic crust. The bolide is a 0.8&thinsp;km diameter basaltic asteroid hitting the Martian surface vertically at a velocity of 12.8&thinsp;km/s. Finally, the numerical results are compared with the MOLA DEM profile in order to analyze the formation mechanism of Martian layered ejecta craters. Our simulations suggest that the presence of an icy layer significantly modifies the cratering mechanics, and many of the unusual features of SLE craters may be explained by the presence of icy layers. Impact cratering on icy satellites is significantly affected by the presence of subsurface H<sub>2</sub>O.

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Eyles, Nick, and Louise Daurio. "Little Ice Age debris lobes and nivation hollows inside Ubehebe Crater, Death Valley, California: Analog for Mars craters?" Geomorphology 245 (September 2015): 231–42. http://dx.doi.org/10.1016/j.geomorph.2015.05.029.

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Jin, Shuanggen, and Tengyu Zhang. "Automatic detection of impact craters on Mars using a modified adaboosting method." Planetary and Space Science 99 (September 2014): 112–17. http://dx.doi.org/10.1016/j.pss.2014.04.021.

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Nimmo, Francis, and Martha S. Gilmore. "Constraints on the depth of magnetized crust on Mars from impact craters." Journal of Geophysical Research: Planets 106, E6 (June 1, 2001): 12315–23. http://dx.doi.org/10.1029/2000je001325.

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VILLIERS, Germari de, David T. KING Jr., and Luke J. MARZEN. "A study of candidate marine target impact craters in Arabia Terra, Mars." Meteoritics & Planetary Science 45, no. 6 (June 2010): 947–64. http://dx.doi.org/10.1111/j.1945-5100.2010.01068.x.

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