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Remote Sensing
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Planetary Geologic Map** and Remote Sensing II
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Planetary Geologic Map** and Remote Sensing II

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: 31 January 2025 | Viewed by 3776

Special Issue Editors

Prof. Dr. Kaichang Di

E-Mail Website
Guest Editor
State Key Laboratory of Remote Sensing Science, Aerospace Information Research Institute, Chinese Academy of Sciences, Bei**g 100101, China
Interests: planetary remote sensing; planetary map**; planetary rover localization and navigation; planetary geomorphology; comparative planetology
Special Issues, Collections and Topics in MDPI journals
Prof. Dr. Long **ao

E-Mail Website
Guest Editor
School of Earth Sciences, China University of Geosciences, Wuhan 430074, China
Interests: planetary geology; planetary geomorphology; extraterrestrial materials; planetary analogs; comparative planetology
Special Issues, Collections and Topics in MDPI journals
Prof. Dr. Jan-Peter Muller

E-Mail Website
Guest Editor
Emeritus Professor, Mullard Space Science Laboratory, Department of Space & Climate Physics, University College London (UCL), Holmbury St Mary RH5 6NT, UK
Interests: deep learning for change detection on Mars; 3D imaging for Mars and the Moon; orbital-rover image fusion; subsurface map**; super-resolution restoration; surface albedo; cloud heights and winds; globe imaging; VR
Special Issues, Collections and Topics in MDPI journals

Special Issue Information

Dear Colleagues,

Planetary geologic maps are spatial and temporal representations of the materials, landforms, structures, and processes of planetary surfaces. Planetary geologic map** is largely based on analyses of various remote sensing data acquired by space missions and is fundamental in understanding the formation and evolution of planetary surfaces and shallow subsurfaces. Planetary remote sensing techniques and the ever-increasing data have greatly supported geologic map**, as well as other scientific studies of the Moon, Mars and other planetary bodies in the solar system.

This is the second edition of the Special Issue “Planetary Geologic Map** and Remote Sensing”.  The first edition was a great success and attracted much attention in the scientific community. Therefore, we are pleased to announce this new volume of Remote Sensing.

We welcome new submissions on the recent advances in planetary geologic map** and planetary remote sensing, including theory, methods, techniques, algorithms, data validation, map** products, and applications. Review articles are also welcome. Articles may address, but are not limited to, the following topics:

  • Planetary geologic map**;
  • Planetary geomorphologic map**;
  • Photogrammetric remote sensing of planetary surfaces;
  • Spectroscopic remote sensing of planetary surfaces;
  • Remote sensing methods, data calibration and validation;
  • Planetary GIS for geologic map**;
  • Recent and future planetary exploration missions;
  • Landing sites studies;
  • Analog studies.

Prof. Dr. Kaichang Di
Prof. Dr. Long **ao
Prof. Dr. Jan-Peter Muller
Guest Editors

Manuscript Submission Information

Manuscripts should be submitted online at mdpi.longhoe.net 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 topography and geomorphology
  • planetary chronology
  • planetary spectrum
  • planetary remote sensing
  • geologic structures
  • geologic map**
  • planetary composition
  • planetary GIS
  • planetary exploration missions
  • landing sites

Related Special Issue

Published Papers (5 papers)

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Research

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19 pages, 22731 KiB  
Article
Study on the Degradation Pattern of Impact Crater Populations in Yutu-2′s Rovering Area
by **nyu Ma, Meixi Chen, Teng Hu, Zhizhong Kang and Meng **ao
Remote Sens. 2024, 16(13), 2356; https://doi.org/10.3390/rs16132356 - 27 Jun 2024
Viewed by 228
Abstract
A detailed analysis of the panoramic camera data from the 27th to 33rd lunar days was conducted on the high-resolution scenes captured by the Yutu-2 rover stations. This analysis aimed to determine the detailed morphological parameters of the 2015 impact craters within the [...] Read more.
A detailed analysis of the panoramic camera data from the 27th to 33rd lunar days was conducted on the high-resolution scenes captured by the Yutu-2 rover stations. This analysis aimed to determine the detailed morphological parameters of the 2015 impact craters within the inspection area. The levels of degradation observed in the impact craters were determined alongside the surface features. Subsequently, the degradation patterns of the impact craters located within the Yutu-2’s roving area and the distribution patterns of the morphological parameters were analysed and investigated. The results of the analysis indicate that 94% of the impact craters exhibited severe degradation, 80% had depth-to-diameter ratios (DDRs) ranging from 0.07 to 0.17, and the remaining craters were moderately degraded. The DDRs of the impact craters exhibited a declining trend with an increase in the dimensions of the impact craters. Additionally, the degree of degradation of impact crater populations demonstrated a decreasing trend. In general, the impact craters along the rover’s route exhibited severe degradation, with the population of degradation degrees gradually decreasing with increasing diameter. Full article
(This article belongs to the Special Issue Planetary Geologic Map** and Remote Sensing II)
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18 pages, 4896 KiB  
Article
Global Inversion of Lunar Surface Oxides by Adding Chang’e-5 Samples
by Shuangshuang Wu, Jian** Chen, Chenli Xue, Yiwen Pan and Cheng Zhang
Remote Sens. 2024, 16(10), 1812; https://doi.org/10.3390/rs16101812 - 20 May 2024
Viewed by 469
Abstract
The chemical distribution on the lunar surface results from the combined effects of both endogenic and exogenic geological processes. Exploring global maps of chemical composition helps to gain insights into the compositional variation among three major geological units, unraveling the geological evolution of [...] Read more.
The chemical distribution on the lunar surface results from the combined effects of both endogenic and exogenic geological processes. Exploring global maps of chemical composition helps to gain insights into the compositional variation among three major geological units, unraveling the geological evolution of the Moon. The existing oxide abundance maps were obtained from spectral images of remote sensing and geochemical data from samples returned by Apollo and Luna, missing the chemical characteristics of the Moon’s late critical period. In this study, by adding geochemical data from Chang’e (CE)-5 lunar samples, we construct inversion models between the Christiansen feature (CF) and oxide abundance of lunar samples using the particle swarm optimization–extreme gradient boosting (PSO-XGBoost) algorithm. Then, new global oxide maps (Al2O3, CaO, FeO, and MgO) and Mg# with the resolution of 32 pixels/degree (ppd) were produced, which reduced the space weathering effect to some extent. The PSO-XGBoost models were compared with partial least square regression (PLSR) models and four previous results, indicating that PSO-XGBoost models possess the capability to effectively describe nonlinear relationships between CF and oxide abundance. Furthermore, the average contents of our results and the Diviner results for 21 major maria demonstrate high correlations, with R2 of 0.95, 0.82, 0.95, and 0.86, respectively. In addition, a new Mg# map was generated, which reveals different magmatic evolutionary processes in the three geologic units. Full article
(This article belongs to the Special Issue Planetary Geologic Map** and Remote Sensing II)
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20 pages, 63242 KiB  
Article
Crater Detection and Population Statistics in Tianwen-1 Landing Area Based on Segment Anything Model (SAM)
by Yaqi Zhao and Hongxia Ye
Remote Sens. 2024, 16(10), 1743; https://doi.org/10.3390/rs16101743 - 14 May 2024
Viewed by 657
Abstract
Crater detection is useful for research into dating a planetary surface’s age and geological map**. The high-resolution imaging camera (HiRIC) carried by the Tianwen-1 rover provides digital image model (DIM) datasets with a resolution of 0.7 m/pixel, which are suitable for detecting meter-scale [...] Read more.
Crater detection is useful for research into dating a planetary surface’s age and geological map**. The high-resolution imaging camera (HiRIC) carried by the Tianwen-1 rover provides digital image model (DIM) datasets with a resolution of 0.7 m/pixel, which are suitable for detecting meter-scale craters. The existing deep-learning-based automatic crater detection algorithms require a large number of crater annotation datasets for training. However, there is currently a lack of datasets of optical images of small-sized craters. In this study, we propose a model based on the Segment Anything Model (SAM) to detect craters in Tianwen-1’s landing area and perform statistical analysis. The SAM network was used to obtain a segmentation mask of the craters from the DIM images. Then non-circular filtering was used to filter out irregular craters. Finally, deduplication and removal of false positives were performed to obtain accurate circular craters, and their center’s position and diameter were obtained through circular fitting analysis. We extracted 841,727 craters in total, with diameters ranging from 1.57 m to 7910.47 m. These data are useful for further Martian crater catalogs and crater datasets. Additionally, the crater size–frequency distribution (CSFD) was also analyzed, indicating that the surface ages of the Tianwen-1 landing area are ~3.25 billion years, with subsequent surface resurfacing events occurring ~1.67 billion years ago. Full article
(This article belongs to the Special Issue Planetary Geologic Map** and Remote Sensing II)
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Review

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31 pages, 93012 KiB  
Review
Water Ice Resources on the Shallow Subsurface of Mars: Indications to Rover-Mounted Radar Observation
by Naihuan Zheng, Chunyu Ding, Yan Su and Roberto Orosei
Remote Sens. 2024, 16(5), 824; https://doi.org/10.3390/rs16050824 - 27 Feb 2024
Viewed by 1343
Abstract
The planet Mars is the most probable among the terrestrial planets in our solar system to support human settlement or colonization in the future. The detection of water ice or liquid water on the shallow subsurface of Mars is a crucial scientific objective [...] Read more.
The planet Mars is the most probable among the terrestrial planets in our solar system to support human settlement or colonization in the future. The detection of water ice or liquid water on the shallow subsurface of Mars is a crucial scientific objective for both the Chinese Tianwen-1 and United States Mars 2020 missions, which were launched in 2020. Both missions were equipped with Rover-mounted ground-penetrating radar (GPR) instruments, specifically the RoPeR on the Zhurong rover and the RIMFAX radar on the Perseverance rover. The in situ radar provides unprecedented opportunities to study the distribution of shallow subsurface water ice on Mars with its unique penetrating capability. The presence of water ice on the shallow surface layers of Mars is one of the most significant indicators of habitability on the extraterrestrial planet. A considerable amount of evidence pointing to the existence of water ice on Mars has been gathered by previous researchers through remote sensing photography, radar, measurements by gamma ray spectroscopy and neutron spectrometers, soil analysis, etc. This paper aims to review the various approaches utilized in detecting shallow subsurface water ice on Mars to date and to sort out the past and current evidence for its presence. This paper also provides a comprehensive overview of the possible clues of shallow subsurface water ice in the landing area of the Perseverance rover, serving as a reference for the RIMFAX radar to detect water ice on Mars in the future. Finally, this paper proposes the future emphasis and direction of rover-mounted radar for water ice exploration on the Martian shallow subsurface. Full article
(This article belongs to the Special Issue Planetary Geologic Map** and Remote Sensing II)
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Other

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14 pages, 21676 KiB  
Technical Note
A Catalogue of Impact Craters and Surface Age Analysis in the Chang’e-6 Landing Area
by Yexin Wang, **g Nan, Chenxu Zhao, Bin **e, Sheng Gou, Zongyu Yue, Kaichang Di, Hong Zhang, **ang** Deng and Shujuan Sun
Remote Sens. 2024, 16(11), 2014; https://doi.org/10.3390/rs16112014 - 4 Jun 2024
Viewed by 432
Abstract
Chang’e-6 (CE-6) is the first sample-return mission from the lunar farside and will be launched in May of 2024. The landing area is in the south of the Apollo basin inside the South Pole Aitken basin. Statistics and analyses of impact craters in [...] Read more.
Chang’e-6 (CE-6) is the first sample-return mission from the lunar farside and will be launched in May of 2024. The landing area is in the south of the Apollo basin inside the South Pole Aitken basin. Statistics and analyses of impact craters in the landing area are essential to support safe landing and geologic studies. In particular, the crater size–frequency distribution information of the landing area is critical to understanding the provenance of the CE-6 lunar samples to be returned and can be used to verify and refine the lunar chronology model by combining with the radioisotope ages of the relevant samples. In this research, a digital orthophoto map (DOM) mosaic with resolution of 3 m/pixel of the CE-6 landing area was generated from the 743 Narrow Angle Camera of the Lunar Reconnaissance Orbiter Camera. Based on the DOM, craters were extracted by an automated method and checked manually. A total of 770,731 craters were extracted in the whole area of 246 km × 135 km, 511,484 craters of which were within the mare area. Systematic analyses of the crater distribution, completeness, spatial density, and depth-to-diameter ratio were conducted. Geologic model age estimation was carried out in the mare area that was divided into three geologic units according to the TiO2 abundance. The result showed that the east part of the mare had the oldest model age of μ3.27−0.045+0.036 Ga, and the middle part of the mare had the youngest model age of μ2.49−0.073+0.072 Ga. The crater catalogue and the surface model age analysis results were used to support topographic and geologic analyses of the pre-selected landing area of the CE-6 mission before the launch and will contribute to further scientific researches after the lunar samples are returned to Earth. Full article
(This article belongs to the Special Issue Planetary Geologic Map** and Remote Sensing II)
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