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High-Resolution Observations of Planetary Geological and Geomorphic Investigation
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High-Resolution Observations of Planetary Geological and Geomorphic Investigation

A special issue of Remote Sensing (ISSN 2072-4292). This special issue belongs to the section "Satellite Missions for Earth and Planetary Exploration".

Deadline for manuscript submissions: closed (31 March 2024) | Viewed by 7012

Special Issue Editors

Dr. Ákos Kereszturi

E-Mail Website
Guest Editor
Research Centre for Astronomy and Earth Sciences, Konkoly Observatory, Budapest, Hungary
Interests: planetary surface geology; fluvial, impact, ice and sedimentary features; comparative geomorphological aspects
Special Issues, Collections and Topics in MDPI journals
Dr. Jiannan Zhao

E-Mail Website
Guest Editor
Key Laboratory of Geological Survey and Evaluation of Ministry of Education, Planetary Science Institute, China University of Geosciences, Wuhan, China
Interests: planetary geology; planetary geomorphology; landing site selection; comparative planetology
Special Issues, Collections and Topics in MDPI journals

Special Issue Information

Dear Colleagues,

As one of the frontier topics of current scientific research, planetary geology and geomorphology exploration have reshaped our understanding of the space world. The continuous improvement of planetary remote sensing technology has greatly supported planetary geology and geomorphology investigation, as well as numerous scientific studies on the Moon, Mars and other planetary bodies in the solar system. It is regarded as one of the indispensable technologies for planetary exploration. Remote sensing data can be used to study planetary surface processes, identify sediments in planetary craters, detect liquid water on Mars, measure space weathering rates, reconstruct geological history, etc.

This Special Issue aims to document expertise in the exploration of all aspects of planetary geology, geomorphology, and landscape evolution through high-resolution observation, as well as contributions to the study of terrestrial planets. Topics include, but are not limited to, planetary geomorphology, planetary surface processes, shallow subsurface tectonics and weathering studies.

Dr. Ákos Kereszturi
Dr. Jiannan Zhao
Guest Editors

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Remote Sensing is an international peer-reviewed open access semimonthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. The Article Processing Charge (APC) for publication in this open access journal is 2700 CHF (Swiss Francs). Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Keywords

  • planetary geology
  • planetary geomorphology
  • planetary landforms
  • planetary surface processes
  • planetary composition
  • planetary geological mapping
  • high-resolution planetary imaging
  • shallow subsurface detection
  • space weathering

Related Special Issue

Published Papers (7 papers)

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17 pages, 5171 KiB  
Article
Interpretation of Geological Features and Volcanic Activity in the Tsiolkovsky Region of the Moon
by Ying Wang, Xiaozhong Ding, Jian Chen, Kunying Han, Chenglong Shi, Ming Jin, Liwei Liu, Xinbao Liu and Jiayin Deng
Remote Sens. 2024, 16(6), 1000; https://doi.org/10.3390/rs16061000 - 12 Mar 2024
Viewed by 695
Abstract
The Tsiolkovsky crater is located on the farside of the Moon. It formed in the late Imbrian epoch and was filled with a large area of mare basalts. Multisource remote sensing data are used to interpret the geological features of the Tsiolkovsky area. [...] Read more.
The Tsiolkovsky crater is located on the farside of the Moon. It formed in the late Imbrian epoch and was filled with a large area of mare basalts. Multisource remote sensing data are used to interpret the geological features of the Tsiolkovsky area. Compared with previous studies, new remote sensing data and a chronological model based on crater size–frequency distribution are used to further refine the stratigraphic units and determine the absolute ages of the mare basalt units. The evolution of volcanic activity in this crater is discussed. The results are as follows: Abundances of major elements, Th, and silicate minerals suggest that the mare basalt in the crater floor is not a uniform unit but rather nine units with different compositions. The nine basalt units are divided into two episodes of volcanic activity: The first occurred at 3.5–3.7 Ga, when highly evolved lava erupted at the crater floor at a large scale; the second occurred at ~3.4 Ga, when a small area of more primitive lava extended to the northern portion of the crater floor. Full article
(This article belongs to the Special Issue High-Resolution Observations of Planetary Geological and Geomorphic Investigation)
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25 pages, 47410 KiB  
Article
Identification of Lunar Craters in the Chang’e-5 Landing Region Based on Kaguya TC Morning Map
by Yanshuang Liu, Jialong Lai, Minggang Xie, Jiannan Zhao, Chen Zou, Chaofei Liu, Yiqing Qian and Jiahao Deng
Remote Sens. 2024, 16(2), 344; https://doi.org/10.3390/rs16020344 - 15 Jan 2024
Viewed by 697
Abstract
Impact craters are extensively researched geological features that contribute to various aspects of lunar science, such as evaluating the model age, regolith thickness, etc. The method for identifying impact craters has gradually transitioned from manual counting to automated identification. Automatic crater detection based [...] Read more.
Impact craters are extensively researched geological features that contribute to various aspects of lunar science, such as evaluating the model age, regolith thickness, etc. The method for identifying impact craters has gradually transitioned from manual counting to automated identification. Automatic crater detection based on the digital elevation model (DEM) is commonly used to detect larger craters. However, using only DEM has limitations in discerning smaller craters (diameter < ~1 km). This study utilizes an improved Faster R-CNN algorithm and the Kaguya Terrain Camera (TC) morning map to detect small impact craters in the Chang’e-5 (CE-5) landing site. It uses model fusion to improve the precision of small crater identification. The results show a recall rate of 96.33% and a precision value of 90.19% for craters with diameters exceeding 200 m. The model found a total of 187,101 impact craters in the CE-5 region. The spatial distribution density of impact craters with diameters ranging from 100 m to 200 m is approximately 2.5706/km2. For craters with diameters ranging from 200 m to 1 km, the average spatial distribution density is about 0.9016/km2. By the unbiased impact crater density of chronological analysis, the model age of the Im2 and Em4 geological units in the CE-5 region is 3.78 Ga and 2.07 Ga, respectively. Full article
(This article belongs to the Special Issue High-Resolution Observations of Planetary Geological and Geomorphic Investigation)
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17 pages, 9388 KiB  
Article
Introduction to Dione’s Wispy Terrain as a Putative Model Region for “Micro” Wilson Cycles on Icy Satellites
by Balázs Bradák, Jun Kimura, Daisuke Asahina, Mayssa El Yazidi and Csilla Orgel
Remote Sens. 2023, 15(21), 5177; https://doi.org/10.3390/rs15215177 - 30 Oct 2023
Cited by 1 | Viewed by 818
Abstract
The Wispy Terrain is the region of chasmata characterized by quasi-parallel fault systems, formed by extensional and shear stresses of the icy crust of Dione, a moon of Saturn. Besides the basic, satellite-scale geological mapping and very general definition of the phenomenon, only [...] Read more.
The Wispy Terrain is the region of chasmata characterized by quasi-parallel fault systems, formed by extensional and shear stresses of the icy crust of Dione, a moon of Saturn. Besides the basic, satellite-scale geological mapping and very general definition of the phenomenon, only a few studies focus on the Wispy Terrain and its chasmata from the angle of detailed tectonic reconstruction, with others mainly targeting, e.g., the timing of its formation. This study provides a detailed geological and cryotectonic analysis in the surroundings of the Eurotas and Palatine Chasmata and proposes additional, until now, unidentified tectonic processes and a formation model. The relationship between fragmentary impact craters and tectonic features indicates other newly suspected tectonic movements, namely thrust, and splay and décollement fault systems. In contrast to the commonly expected and identified dilatational processes, such fault types show compression and are characteristic of subduction in a terrestrial environment. Theoretically, the appearance of such tectonic processes means that the already-known rift and the newly discovered subsumption (subduction-like) processes may appear together in the Wispy Terrain. The appearance of both features may suggest the presence of some of the components (phases) of a Wilson cycle analog cryotectonic cycle (or possibly cycles) in icy planetary bodies like Dione. Full article
(This article belongs to the Special Issue High-Resolution Observations of Planetary Geological and Geomorphic Investigation)
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23 pages, 21658 KiB  
Article
Geometric Accuracy Analysis of Regional Block Adjustment Using GF-7 Stereo Images without GCPs
by Xinming Tang, Xiaoyong Zhu, Wenmin Hu and Jianhang Ding
Remote Sens. 2023, 15(10), 2552; https://doi.org/10.3390/rs15102552 - 12 May 2023
Viewed by 825
Abstract
As an important means of improving positioning accuracy, block adjustment has been used in the improvement and assessment of accuracy for the Chinese Gaofen-7 (GF-7) satellite. However, there is little research on what factors affect accuracy without ground control points (GCPs). The correlation [...] Read more.
As an important means of improving positioning accuracy, block adjustment has been used in the improvement and assessment of accuracy for the Chinese Gaofen-7 (GF-7) satellite. However, there is little research on what factors affect accuracy without ground control points (GCPs). The correlation between accuracy and the images participating in the adjustment is not clear. This paper proposes the correlation coefficients and canonical correlation analysis between five accuracy indicators and three sets of ten adjustment factors, including topographic factors, participating image factors, and tie points (TPs) factors, to quantify the influence of adjustment factors on accuracy. Block adjustment without GCPs for GF-7 stereo imagery is verified in three study areas to evaluate the relationship between accuracy and adjustment factors. The results show that block adjustment without GCPs can improve direct positioning accuracy with an average improvement of 1.27 m in the planar direction and 0.13 m in the elevation direction. Moreover, plane accuracy is more easily affected by three sets of factors, while the influence on elevation accuracy is more balanced. The set of TP factors has the greatest influence on accuracy, and the image overlap is more critical than the image coverage area, number, and time periods. Topographic factors also play an important role, and the influence of the elevation factor with the highest canonical correlation coefficient (−0.71) is more significant than the other two factors, roughness, and slope. The results provide a reference for the improvement of adjustment accuracy without GCPs, the reasonable selection of adjustment images, the optimization of TPs, and the strategy of the partition processing of large-area block adjustment for GF-7 stereo imagery. Full article
(This article belongs to the Special Issue High-Resolution Observations of Planetary Geological and Geomorphic Investigation)
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17 pages, 24095 KiB  
Article
Comparison of Topographic Roughness of Layered Deposits on Mars
by Wei Cao, Zhiyong Xiao, Fanglu Luo, Yizhen Ma and Rui Xu
Remote Sens. 2023, 15(9), 2272; https://doi.org/10.3390/rs15092272 - 25 Apr 2023
Cited by 1 | Viewed by 1196
Abstract
Impact craters with layered ejecta deposits are widespread on Mars. Prevailing views suggest that such ejecta were formed due to the involvement of target water and/or water ice in the impact excavation and/or the post-deposition movement of the impact ejecta. The long-runout landslides [...] Read more.
Impact craters with layered ejecta deposits are widespread on Mars. Prevailing views suggest that such ejecta were formed due to the involvement of target water and/or water ice in the impact excavation and/or the post-deposition movement of the impact ejecta. The long-runout landslides and lobate debris aprons that are likely formed due to the involvement of water ice are used as analogs to compare roughness at multiple scales, considering that these three landforms share some similarities in their geomorphology. Analog studies of the morphological similarities and differences of layered ejecta deposits with different emplacement mechanisms are an important approach to untangling how layered ejecta deposits might form on Mars and beyond. Earlier morphological comparisons were usually based on qualitative descriptions or one-dimensional topographic roughness characteristics at given azimuths; however, the emplacement processes of layered deposits are recorded in two-dimensional topography and at multiple scales. In this study, we designed a multiwavelet algorithm to characterize the multi-scale topographic roughness of different forms of Martian layered deposits. Our comparisons show that the inner facies of the layered ejecta deposits and long-runout landslides exhibited similar roughness characteristics, and the outer facies of the layered ejecta deposits were more similar in roughness to lobate debris aprons. This study highlights the importance of the spatial resolution of digital terrain models in characterizing fine topographic fluctuations on layered ejecta deposits, providing additional insights into the possible emplacement mechanisms of different parts of layered ejecta deposits. Full article
(This article belongs to the Special Issue High-Resolution Observations of Planetary Geological and Geomorphic Investigation)
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33 pages, 8870 KiB  
Article
Major Elements Concentrations in Chang’E-3 Landing Site from Active Particle-Induced X-ray Spectrometer
by Man-Hei Ng, Xiaoping Zhang, Yi Xu and Liansheng Li
Remote Sens. 2023, 15(6), 1643; https://doi.org/10.3390/rs15061643 - 18 Mar 2023
Viewed by 1254
Abstract
On 14 December 2013 (UTC), China’s Chang’E-3 (CE-3) succeeded in landing on the Moon’s surface. The CE-3 landing site is in northern Mare Imbrium and several tens of meters away from the rim of a young crater with a few hundred meters in [...] Read more.
On 14 December 2013 (UTC), China’s Chang’E-3 (CE-3) succeeded in landing on the Moon’s surface. The CE-3 landing site is in northern Mare Imbrium and several tens of meters away from the rim of a young crater with a few hundred meters in diameter. In-situ measurements of lunar soil around the roving area were conducted from Active Particle-induced X-ray Spectrometer (APXS) onboard Yutu rover. Three relatively young lunar soil samples in the CE-3 landing site were investigated. Previous studies suggested that these samples are a new type of basalt, not discovered yet in previous missions before the CE-3 in-situ measurements. It plays an essential role in promoting the understanding of lunar volcanic history. However, their results are deviated, and thus scrutinizing the data as per our optimized model to derive a more precise result is of necessity. In this paper, we present an optimized model for data analysis based on APXS measurements to derive the major elements concentrations. The optimized model has the advantages of reliability and being independent of calibration by ground standards. The particle size effect is applied in lunar X-ray fluorescence modeling for correction, improving the accuracy in determining the elemental concentrations for the actual measurement. Our results are distinct in the correlation plots by carrying out a comparison with previous lunar regolith samples from Apollo, Luna, and Chang’E-5 missions, indicating that the CE-3 landing site is a new region apart from previous in-situ or laboratory detection prior to the CE-3 measurements. It suggests a kind of young mare basalt with unusual petrological characteristics compared with previous samples and similar geochemical properties of CE-3 landing site and western Procellarum and Imbrium (WPI), with a signature of western Procellarum. Full article
(This article belongs to the Special Issue High-Resolution Observations of Planetary Geological and Geomorphic Investigation)
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14 pages, 4497 KiB  
Technical Note
Mapping Cones on Mars in High-Resolution Planetary Images with Deep Learning-Based Instance Segmentation
by Chen Yang, Nan Zhang, Renchu Guan and Haishi Zhao
Remote Sens. 2024, 16(2), 227; https://doi.org/10.3390/rs16020227 - 06 Jan 2024
Viewed by 785
Abstract
Cones are among the significant and controversial landforms on Mars. Martian cones exhibit various morphological characteristics owing to their complex origin, and their precise origin remains an active research topic. A limited number of cones have been manually mapped from high-resolution images in [...] Read more.
Cones are among the significant and controversial landforms on Mars. Martian cones exhibit various morphological characteristics owing to their complex origin, and their precise origin remains an active research topic. A limited number of cones have been manually mapped from high-resolution images in local areas, and existing detection methods are only applicable to a single type of cone that has a similar morphology and spatial distribution, leading to the vast majority remaining unidentified. In this paper, a novel cone identification approach is proposed that is specially designed for adequately recognizing cones from different regions in high-resolution planetary images. First, due to the lack of a publicly available cone database for reference, we annotated 3681 cones according to the literature on manual interpretation and the cone information provided by the Lunar and Planetary Laboratory (IRL) in HiRISE images. Then, the cone identification problem was converted into an instance segmentation task, i.e., a cone identification approach was designed based on deep neural networks. The Feature Pyramid Network-equipped Mask R-CNN was utilized as the detection and segmentation model. Extensive experiments were conducted for fine recognition of Martian cones with HiRISE. The results show that the proposed approach achieves high performance; it especially efficiently detects multiple types of cones while generating accurate segmentation to describe the geometry contour of cones. Finally, a Martian cone dataset with deep learning-based instance segmentation (DL-MCD) was built, containing 3861 cones for exploring geological processes on the surface of Mars. Full article
(This article belongs to the Special Issue High-Resolution Observations of Planetary Geological and Geomorphic Investigation)
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