Journal of Geophysical Research: Planets最新文献

{"title":"Stability and Collapse Analysis of Terrestrial Lava Tubes Under Irregular Shapes: Case Study of Skull and Valentine Caves","authors":"Marcin Chwała,&nbsp;Maciej Bodlak,&nbsp;Patrick Whelley","doi":"10.1029/2025JE009109","DOIUrl":"10.1029/2025JE009109","url":null,"abstract":"<p>Lava tubes have attracted increasing attention from scientists and space industry professionals due to their potential as protective shelters on planetary bodies such as the Moon or Mars as well as for scientific research. This interest has motivated investigations into terrestrial lava tubes as analogs for extraterrestrial caves. In this study, we present the first comprehensive numerical analysis of the stability and collapse geometry of two terrestrial lava tubes, Skull Cave and Valentine Cave, using laser scan data of their interiors and surrounding terrain. Our methodology is based on finite element limit analysis, which can accurately and efficiently replicate the natural and irregular shapes of these caves for stability analysis. We performed additional analyses by varying rock roof thickness and other parameters to validate whether previous findings from studies on artificially generated irregular shapes hold true for actual cave geometries. Our results provide new insights into how natural irregularities in cave geometry influence stability and collapse mechanisms. The results confirm the significant impact of these irregularities and offer a robust approach for assessing cave stability.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 8","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-08-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144881315","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Dynamos Driven by Top-Heavy Double-Diffusive Convection in the Strong-Field Regime","authors":"Wei Fan,&nbsp;Yufeng Lin","doi":"10.1029/2025JE008969","DOIUrl":"10.1029/2025JE008969","url":null,"abstract":"<p>The magnetic fields of terrestrial planets are generated in their liquid cores through dynamo action driven by thermal and compositional convection. The coexistence of these two buoyancy sources gives rise to double-diffusive convection (DDC) due to the contrast between thermal and compositional diffusivities. However, most dynamo simulations adopt the co-density model, where the two diffusivities are assumed to be equal. In this study, we performed both hydrodynamic and dynamo simulations of top-heavy DDC in a rotating spherical shell with the Lewis number <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>L</mi>\u0000 <mi>e</mi>\u0000 <mo>=</mo>\u0000 <mn>100</mn>\u0000 </mrow>\u0000 <annotation> $Le=100$</annotation>\u0000 </semantics></math>, and compared them with corresponding co-density models. In the hydrodynamic regime, the convective flow morphology is strongly influenced by the nature of the buoyancy sources. However, our dynamo simulations in the strong-field regime demonstrate that the co-density and DDC models yield qualitatively similar magnetic fields at comparable magnetic Reynolds numbers, albeit with some differences in detail. These numerical models further justify the use of the co-density model in planetary dynamo simulations. Finally, we demonstrate that dynamo models based on DDC and co-density produce similar magnetic fields and secular variations at the core-mantle boundary. This suggests that it may not be possible to distinguish the buoyancy sources responsible for planetary dynamos based solely on magnetic field observations.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 8","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-08-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144881094","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Monte Carlo Simulation of the Global Migration of Lunar Hydroxyl From a Magnetic-Shielded Solar Wind Source","authors":"Jundi Chen,&nbsp;Lianghai Xie,&nbsp;Lei Li,&nbsp;Yang Liu,&nbsp;Aibing Zhang,&nbsp;Yiteng Zhang,&nbsp;Jiannan Li,&nbsp;Yuchen Xu,&nbsp;Jindong Wang,&nbsp;Yazhou Yang,&nbsp;Bin Zhou,&nbsp;Qi Yan,&nbsp;Qi Xu,&nbsp;Xiaochen Gou,&nbsp;Yongyong Feng,&nbsp;Tianhua Zhong,&nbsp;Chi Wang","doi":"10.1029/2025JE009003","DOIUrl":"10.1029/2025JE009003","url":null,"abstract":"&lt;p&gt;Solar wind has been regarded as an important source for the surficial water on the Moon. Here we investigate the global migration of solar wind-derived hydroxyl (OH) molecules with a Monte Carlo model, in which the shielding effects of both the Earth's magnetosphere and the lunar magnetic anomalies on the production rate of OH are considered. It is found that the OH surface concentration depends on the latitude, the local time, and the lunar phase. Specifically, the surface concentration can increase from nearly zero ppm near the subsolar point to about 1,000 ppm near the polar regions, and there is a local peak near the morning terminator that can result in a diurnal variation of about 100 ppm. Moreover, the OH abundances can be reduced by about 15% in the magnetotail when at low and mid latitudes. But when in the polar region, the OH abundance can keep increasing, resulting in an average deposition rate of &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mn&gt;1.0&lt;/mn&gt;\u0000 &lt;mo&gt;×&lt;/mo&gt;\u0000 &lt;msup&gt;\u0000 &lt;mn&gt;10&lt;/mn&gt;\u0000 &lt;mn&gt;12&lt;/mn&gt;\u0000 &lt;/msup&gt;\u0000 &lt;mspace&gt;&lt;/mspace&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;m&lt;/mi&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;2&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/msup&gt;\u0000 &lt;mspace&gt;&lt;/mspace&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;s&lt;/mi&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;1&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/msup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; $1.0times {10}^{12} {mathrm{m}}^{-mathrm{2}} {mathrm{s}}^{-mathrm{1}}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;. In addition, a south-north asymmetry can be caused by the magnetic anomalies, in which the OH abundance in the southern hemisphere is generally lower than that in the northern hemisphere, with maximum difference of about 31% near the 75° latitude. In the exosphere, the OH number density shows a dawn-dusk asymmetry, with relatively higher number densities on the dawnside, and the maximum density can reach &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mn&gt;2.8&lt;/mn&gt;\u0000 &lt;mo&gt;×&lt;/mo&gt;\u0000 &lt;msup&gt;\u0000 &lt;mn&gt;10&lt;/mn&gt;\u0000 &lt;mn&gt;9&lt;/mn&gt;\u0000 &lt;/msup&gt;\u0000 &lt;mspace&gt;&lt;/mspace&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;m&lt;/mi&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mn&gt;3&lt;/mn&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/msup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; $2.8times {10}^{9} {mathrm{m}}^{-mathrm{3}}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; near the subsolar region. These results can greatly improve our understanding on the migration and distribution of OH molecules on the ","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 8","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-08-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144869836","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Observation of Water Ice Halos and Bright Cores Within Dark Dune Spots on Mars: Implication for a Solid Greenhouse Effect","authors":"J. Peng,&nbsp;L. Pan,&nbsp;A. Lucchetti","doi":"10.1029/2024JE008813","DOIUrl":"10.1029/2024JE008813","url":null,"abstract":"<p>Dark dune spots are seasonal low albedo features observed in the Martian polar regions. A formation mechanism of gas jets has been proposed for the formation of dark dune spots. However, the composition and state of the volatile species involved remain debated. Here we report the observations of dark central deposits, bright halos and cores within dark dune spots using the High-Resolution Imaging Science Experiment images. Time series observations show that after the disappearance of bright halos, the bright cores are later exposed on the surface as a result of the removal of the dark deposits above. The Compact Reconnaissance Imaging Spectrometer data analysis suggests that the bright halos consist of a combination of H₂O and CO₂ ice. During the season when bright cores are observed, water-ice halos have disappeared and the diurnal maximum temperature is up to 278K, close to the sublimation point of H₂O ice. Both the spectral data and surface temperature suggest a significant role of H₂O ice during the formation of dark dune spots. We propose that the subsurface heating of a chamber filled with H₂O ice under the seasonal CO₂ ice slab resulted in the phase change of H₂O ice during the evolution of dark dune spots, which has been proposed as the solid-state greenhouse effect (Matson &amp; Brown, 1989, https://doi.org/10.1016/0019-1035(89)90007-9). The results suggest a relatively mild environment with raised temperature and pressure compared to the Martian surface under the seasonal ice caps in the south polar regions of Mars.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 8","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-08-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144869837","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Tectonic History and Seismicity in the Lunar North Polar Region: New Insights From the Geometry, Kinematics, Resurfacing Ages, and Seismic Hazard Potential of Lobate Scarps","authors":"Abhisek Mishra,&nbsp;P. Senthil Kumar","doi":"10.1029/2024JE008639","DOIUrl":"10.1029/2024JE008639","url":null,"abstract":"<p>Lunar surface manifested a variety of tectonic structures in which lobate scarps (shallow thrust faults) are wide-spread globally. Despite many previous studies, the formation characteristics of lobate scarps in the lunar polar regions are poorly known. Earlier, we studied the geometry, kinematics, formation ages and seismic hazard potential of scarps in the lunar south polar region. In this study, we focused on the lunar north polar region, where we newly detected &gt;280 individual lobate scarp segments and characterized their morphologic properties and formation ages. Orientations and movement directions of these scarps show spatial and latitudinal variations. Many scarps show pole-ward movements. We dated 105 scarp segments using the conventional crater counting method. Counting of fresh craters on these scarps yielded a majority age range of 4.8–75 Ma, while counting of all craters yielded 11–470 Ma range. These are interpreted to be the resurfacing ages of scarps due to seismic resetting, which occurred mostly in the last 100 million years. The fault ages indicate contemporaneous tectonic activity in different parts of the polar region. The lengths of majority scarp segments indicate their shallower fault depths (∼1 km) that are capable of producing small to medium size shallow moonquakes. The epicentral distances of many shallow moonquakes detected from the Apollo data coincide with the north polar lobate scarps. Considering <i>M</i>_W 1–4 shallow moonquakes along the lobate scarps, we provided a deterministic seismic hazard scenario. We conclude that lobate scarps in the lunar polar regions have a contrasting spatial distribution pattern and kinematic properties.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 8","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-08-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144861729","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"An Observational Overview of the Ubiquitous Dust Tides in the Martian Atmosphere","authors":"Zhaopeng Wu,&nbsp;Jing Li,&nbsp;Tao Li,&nbsp;Yueming Cheng,&nbsp;Jun Cui,&nbsp;Chengyun Yang,&nbsp;Zhaojin Rong,&nbsp;Fei He,&nbsp;Xuan Cheng,&nbsp;Yong Wei","doi":"10.1029/2025JE008971","DOIUrl":"10.1029/2025JE008971","url":null,"abstract":"<p>Dust activity on Mars is not physically different in nature from that on Earth, except that it is more intense and critical to the Martian climate under the specific planetary and atmospheric parameters of Mars. Previously found atmospheric dust tides during large Martian dust storms are a significant short-term global-scale dust activity, analogous to Earth's ocean tides. However, it is not certain whether dust tides are widespread on Mars. In this paper, we use multi-local time observations of Martian year (MY) 33 from the Mars Climate Sounder to provide the first detailed overview of dust tides over the entire MY. We generalize two scenarios of dust tides from the spatial distribution of the day-night difference of dust, called the low-latitude scenario and the low-altitude scenario, respectively. The two scenarios are ubiquitous and show distinct seasonal variations. For the first time, we find a downward phase progression signal in the atmospheric dust abundance, similar to the vertical propagation of thermal tides, providing direct evidence for the role of vertically propagated thermal tides in driving the diurnal variations of dust. Utilizing the Lagrangian particle simulation, we show that the diurnal dust motion in both scenarios is driven by meridional and vertical tidal winds. This implies that the associated wind fields can be inferred inversely from the diurnal variations of the airborne dust and can be used to indirectly estimate global wind fields. The relatively simple Martian atmosphere could also be used to test and advance existing theories of Earth's dust activity.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 8","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-08-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144861728","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Automatic Classification of Primary and Secondary Craters Near Copernicus Crater With Updated Insights on Its Impact Trajectory and Age","authors":"Yiran Wang,&nbsp;Miao Zhuo,&nbsp;Bo Wu,&nbsp;Shuo Liu,&nbsp;Dijun Guo","doi":"10.1029/2024JE008516","DOIUrl":"10.1029/2024JE008516","url":null,"abstract":"<p>Impact cratering is the dominant geological process shaping the Moon's surface. Primary craters form from direct asteroid or comet impacts, while secondary craters are created by debris ejected from these primary impacts. Accurately identifying secondary craters within the primary crater population is essential for understanding planetary processes and surface ages. However, manually distinguishing these secondary craters can be time-consuming and challenging. In this work, a statistical analysis of 5,460 primary and secondary craters reveals significant differences in their spectral characteristics. These differences are postulated to originate from distinct degrees of modification to the target materials and weathering processes. Employing a deep learning model, the research specifically targets the Copernicus crater region to automate the identification of secondary craters. The model classified ∼285,000 secondary and ∼39,000 primary craters with diameters from 200 m to 5 km. Secondary craters make up 89% of the total at 200–280 m, decreasing to around 65% at 4,520–5,000 m. The azimuthal distribution of identified secondary craters suggests an oblique impact from southeast to northwest that formed the Copernicus crater. The model age, based on craters superposed on the ejecta, estimates the Copernicus crater to be ∼755 Ma, overlaying a 3.69 Ga surface. The estimated ages align with previous research. The method is best suited for geologically homogeneous, airless surfaces, and is limited when older primary craters are buried by later ejecta or when ancient craters exhibit similar spectral features due to degradation.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 8","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-08-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144853654","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Statistical Methods to Distinguish Shallow Moonquakes From Impacts","authors":"Alice R. Turner,&nbsp;Sean P. S. Gulick,&nbsp;Daniel T. Trugman,&nbsp;Francesco Civilini,&nbsp;Keisuke Onodera","doi":"10.1029/2024JE008739","DOIUrl":"10.1029/2024JE008739","url":null,"abstract":"<p>One of the biggest challenges in lunar seismology is accurately classifying seismic signals to evaluate impact and seismicity rates. While past studies have used qualitative differences for classification, we introduce quantitative methods to distinguish the most energetic signals: shallow moonquakes and natural impacts. Our approach utilizes previously under-analyzed data from the short-period Apollo seismic instruments, which operated on the Moon between 1969 and 1977. First, we convert short-period spectrograms to smoothed probability density functions. Next, we use the Kullback–Leibler divergence as a metric to measure the differences in the spectrograms between the two types of event. Using this comparison metric, we find that shallow moonquakes are more similar to other shallow moonquakes than to impacts. By analyzing individual waveforms, we identify features that significantly differ between shallow moonquakes and impacts, such as spectral entropy and autocorrelation. These features, which have characteristic ranges of values for each class of event, can be used to categorize the signal without comparison to another event. We apply these statistical metrics to a set of previously unclassified high-frequency events and shallow moonquakes that were identified last year. We find that high-frequency events and newly identified shallow moonquakes have a variety of features. Many of the shallow moonquakes that were identified last year are consistent with those identified over 50 years ago and may have a range of source depths. Along with supporting reanalysis of the Apollo seismic signals, these statistical metrics may be useful for future analysis of lunar seismic data.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 8","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-08-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008739","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144843274","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Role of Reducing and Acidic Hydrothermal Fluids in Forming Chloride Deposits in Terra Sirenum, Mars","authors":"David C. Fernández-Remolar,&nbsp;Wladyslaw Altermann,&nbsp;David Gomez-Ortiz,&nbsp;Brian Hynek,&nbsp;Matthew R. M. Izawa,&nbsp;Ernst Hauber,&nbsp;Solmaz Adeli,&nbsp;Ricardo Amils,&nbsp;Ting Huang,&nbsp;Nigel Blamey,&nbsp;Angelo Pio Rossi,&nbsp;Laetitia Le Deit","doi":"10.1029/2024JE008837","DOIUrl":"10.1029/2024JE008837","url":null,"abstract":"<p>Orbital remote sensing has shown that some regions of the ancient Martian crust contain hundreds of discrete terrains covered by chloride-rich evaporites. In terrestrial evaporitic systems, evaporite sequences typically begin with the deposition of carbonates, followed by sulfates, and finally chlorides, a depositional sequence that has not yet been found on Mars. Instead, sulfate deposits are always separated spatially and temporally from chlorides, suggesting two different depositional regimes. Here, we present a model driven by the Martian chlorine geochemical cycle that allows the formation of chlorides whilst simultaneously inhibiting sulfate and carbonate precipitation. In this model, the chlorides are produced under reducing and acidic conditions. Chloride deposition was driven by hydrothermal alteration of the Martian crust associated with faults, followed by precipitation from ascending saline solutions along the tectonic conduits. These processes occurred under a relatively thick and reducing atmosphere (1–0.1 bar). The crustal circulation of chloride-precipitating fluids may have been driven by tectonic suction and pumping processes. Parental brines from hydrothermal activity sourcing chloride might also have contributed to the sulfates found in Cross and Columbus craters of Terra Sirenum. Our study integrates orbital imaging, topography, and spectroscopy with geochemical modeling and terrestrial analogs. We propose that the Terra Sirenum chloride deposits derive from subsurface brines, with deposition driven using tectonic and hydrothermal processes. Under inferred reducing and anoxic conditions, chloride formed with minimal co-precipitation of sulfates and carbonates. Unlike isolated chloride deposits confined to topographic lows, the Terra Sirenum chlorides are associated with linear features interpreted as faults.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 8","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145128992","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"An Integrated Remote Sensing Lineament Investigation of the Manicouagan Region, Canada: Implications for Planetary Cratering Processes","authors":"Mary-Anne Fobert,&nbsp;John G. Spray,&nbsp;Vernon Singhroy","doi":"10.1029/2025JE008982","DOIUrl":"10.1029/2025JE008982","url":null,"abstract":"<p>Remote sensing data were deployed to create a lineament map (LM) of central Quebec, Canada. The LM provides a first-order representation of the geological structures and is shown to co-align with 45% of the structural features previously mapped in the area. Areas displaying partial or no alignment are attributed to inconsistent structural surficial expressions, indistinguishable edge gradients, obscurity by water, and spatial offsets. Despite these challenges, the LM has extended published structural features and extracted a substantial number of new linear features. The LM allows for the distinction between pre-impact regional features from those generated by the Manicouagan impact event. Pre-impact fault systems facilitated a polygonal form to the structure, rendering Manicouagan a polygonal impact crater. Combined with field-based constraints, the LM results also reveal that the crater shows structural asymmetry, with more damage in the SW sector, expressed by enhanced concentric and radial faulting, and an elliptical collapsed transient cavity (orientated ∼70 km NE-SW and 85 km NW-SE). In addition, the central uplift is offset uprange from the geometric center to the NE and the central peak is breached, with a deeper footwall trench opening downrange to the SW. These observations indicate that Manicouagan may have been formed by a projectile traveling with a trajectory from the present-day NE at an oblique angle. The distinction of pre-impact target structures from impact-generated features on Earth has implications for better understanding these features on other solid planetary bodies, comparisons with which are made from craters on the Moon, Mars and Mercury.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 8","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE008982","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145128956","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}