Pub Date : 2025-04-01Epub Date: 2025-02-07DOI: 10.1016/j.pss.2025.106062
A.A. Alves , V. Carruba , E.M.D.S. Delfino , V.R. Silva , L. Blasco
Secular resonances occur when there is a commensurability between the fundamental frequencies of asteroids and planets. These interactions can affect orbital elements like eccentricity and inclination. In this work, our focus is to study the resonance, which affects highly inclined asteroids in the inner main belt around the Phocaea family. Traditionally, the identification of these asteroids was done manually, which demanded a significant amount of time and became unfeasible due to the large volume of data. Our goal is to develop deep learning models for the automatic identification of asteroids affected by this resonance. In this work, Convolutional Neural Network (CNN) models, such as VGG, Inception, and ResNet, as well as the Vision Transformer (ViT) architecture, are used. To evaluate the performance of the models, we used metrics such as accuracy, precision, recall, and F1-score, applied to both filtered and unfiltered elements. We applied deep learning methods and evaluated which one presented the best effectiveness in the classification of asteroids affected by the secular resonance. To improve the performance of the models, we employed regularization techniques, such as data augmentation and dropout. CNN models demonstrated excellent performance with both filtered and unfiltered elements, but the Vision architecture stood out, providing exceptional performance across all used metrics and low processing times.
{"title":"Deep learning identification of asteroids interacting with g-s secular resonances","authors":"A.A. Alves , V. Carruba , E.M.D.S. Delfino , V.R. Silva , L. Blasco","doi":"10.1016/j.pss.2025.106062","DOIUrl":"10.1016/j.pss.2025.106062","url":null,"abstract":"<div><div>Secular resonances occur when there is a commensurability between the fundamental frequencies of asteroids and planets. These interactions can affect orbital elements like eccentricity and inclination. In this work, our focus is to study the <span><math><mrow><mi>g</mi><mo>−</mo><msub><mrow><mi>g</mi></mrow><mrow><mn>6</mn></mrow></msub><mo>−</mo><mi>s</mi><mo>+</mo><msub><mrow><mi>s</mi></mrow><mrow><mn>6</mn></mrow></msub></mrow></math></span> resonance, which affects highly inclined asteroids in the inner main belt around the Phocaea family. Traditionally, the identification of these asteroids was done manually, which demanded a significant amount of time and became unfeasible due to the large volume of data. Our goal is to develop deep learning models for the automatic identification of asteroids affected by this resonance. In this work, Convolutional Neural Network (CNN) models, such as VGG, Inception, and ResNet, as well as the Vision Transformer (ViT) architecture, are used. To evaluate the performance of the models, we used metrics such as accuracy, precision, recall, and F1-score, applied to both filtered and unfiltered elements. We applied deep learning methods and evaluated which one presented the best effectiveness in the classification of asteroids affected by the secular resonance. To improve the performance of the models, we employed regularization techniques, such as data augmentation and dropout. CNN models demonstrated excellent performance with both filtered and unfiltered elements, but the Vision architecture stood out, providing exceptional performance across all used metrics and low processing times.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"258 ","pages":"Article 106062"},"PeriodicalIF":1.8,"publicationDate":"2025-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143395582","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-04-01Epub Date: 2025-02-20DOI: 10.1016/j.pss.2025.106076
John R. Marshall , Lori K. Fenton
On Saturn's moon Titan the unique combination of low gravity, low-density surface materials (ices), and high atmospheric density may enable the wind to roll pebble, cobble, and perhaps even small boulder-size stones. If so, Titan's aeolian environment would be unlike that of Earth or Mars where wind is generally limited to transporting sand and dust much less than a couple of millimeters in size. To investigate the rolling-stone possibility we conducted a mathematical analysis constrained by conventional engineering and aerodynamic theory. We show that the minimum wind strength to cause saltation of sand on Titan is sufficient, under certain geological conditions, to also roll stones as large as ∼0.5 m diameter. Various features previously mapped on Titan have characteristics consistent with fields of wind-rolled stones, with the most compelling candidate being radar-bright ‘streak-like plains’ that are elongated parallel to nearby linear dunes. Possible implications for Titan science and the Dragonfly mission are considered.
{"title":"Rolling stones on Titan","authors":"John R. Marshall , Lori K. Fenton","doi":"10.1016/j.pss.2025.106076","DOIUrl":"10.1016/j.pss.2025.106076","url":null,"abstract":"<div><div>On Saturn's moon Titan the unique combination of low gravity, low-density surface materials (ices), and high atmospheric density may enable the wind to roll pebble, cobble, and perhaps even small boulder-size stones. If so, Titan's aeolian environment would be unlike that of Earth or Mars where wind is generally limited to transporting sand and dust much less than a couple of millimeters in size. To investigate the rolling-stone possibility we conducted a mathematical analysis constrained by conventional engineering and aerodynamic theory. We show that the minimum wind strength to cause saltation of sand on Titan is sufficient, under certain geological conditions, to also roll stones as large as ∼0.5 m diameter. Various features previously mapped on Titan have characteristics consistent with fields of wind-rolled stones, with the most compelling candidate being radar-bright ‘streak-like plains’ that are elongated parallel to nearby linear dunes. Possible implications for Titan science and the Dragonfly mission are considered.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"258 ","pages":"Article 106076"},"PeriodicalIF":1.8,"publicationDate":"2025-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143488290","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-01Epub Date: 2025-01-22DOI: 10.1016/j.pss.2025.106049
Eulogio Pardo-Igúzquiza , Peter Dowd
This paper provides a new view of the lunar surface by using maps of its closed depressions which are not limited to impact craters. On the lunar landscape, in addition to impact craters of all sizes, there is a rich variety of other types of closed depressions related to impact, volcanism, tectonics and gravitational processes. Kilometre-scale closed depressions have been identified, delineated and mapped on the surface of the Moon by using the digital elevation model provided by the Lunar Orbiter Laser Altimeter (LOLA) instrument onboard the Lunar Reconnaissance Orbiter (LRO) spacecraft together with a pit filling algorithm. The map of closed depressions is a raster map of the same size and spatial resolution as the digital elevation model used to generate it and each pixel provides the depth with respect to the rim of the depression. A number of test sites were chosen to illustrate the methodology including impact basins, maria, highlands, volcanic terrain, intermediate terrain and modified terrain. These maps of closed depressions can be analysed in terms of their location, abundance, size, orientation, depth, geometry, asymmetry and irregularity together with other morphometric parameters. On average, 71% of the surface of the Moon is covered by closed depressions and that number decreases to around 55% for volcanic terrains. The histogram of the depths of the highlands test site can be considered as the standard depth histogram in which impact craters of all sizes cover the entire terrain. The histograms of the other zones vary from that standard profile. The ultimate purpose of this paper is to provide a tool for mapping closed-depressions on the lunar surface which may assist planetary geologists to identify geological processes and recognize geological formations in the study of the geology and geomorphology of the Moon.
{"title":"Closed depressions on the surface of the Moon","authors":"Eulogio Pardo-Igúzquiza , Peter Dowd","doi":"10.1016/j.pss.2025.106049","DOIUrl":"10.1016/j.pss.2025.106049","url":null,"abstract":"<div><div>This paper provides a new view of the lunar surface by using maps of its closed depressions which are not limited to impact craters. On the lunar landscape, in addition to impact craters of all sizes, there is a rich variety of other types of closed depressions related to impact, volcanism, tectonics and gravitational processes. Kilometre-scale closed depressions have been identified, delineated and mapped on the surface of the Moon by using the digital elevation model provided by the Lunar Orbiter Laser Altimeter (LOLA) instrument onboard the Lunar Reconnaissance Orbiter (LRO) spacecraft together with a pit filling algorithm. The map of closed depressions is a raster map of the same size and spatial resolution as the digital elevation model used to generate it and each pixel provides the depth with respect to the rim of the depression. A number of test sites were chosen to illustrate the methodology including impact basins, maria, highlands, volcanic terrain, intermediate terrain and modified terrain. These maps of closed depressions can be analysed in terms of their location, abundance, size, orientation, depth, geometry, asymmetry and irregularity together with other morphometric parameters. On average, 71% of the surface of the Moon is covered by closed depressions and that number decreases to around 55% for volcanic terrains. The histogram of the depths of the highlands test site can be considered as the standard depth histogram in which impact craters of all sizes cover the entire terrain. The histograms of the other zones vary from that standard profile. The ultimate purpose of this paper is to provide a tool for mapping closed-depressions on the lunar surface which may assist planetary geologists to identify geological processes and recognize geological formations in the study of the geology and geomorphology of the Moon.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106049"},"PeriodicalIF":1.8,"publicationDate":"2025-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284559","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-01Epub Date: 2025-01-27DOI: 10.1016/j.pss.2025.106050
A.S. Shimolina , R.E. Ernst , H. El Bilali , D.G. Malyshev , V.E. Rozhin , E.G. Antropova
Theia Mons (centered at 23.4° N, 79.4° W) is the main volcanic center for the Beta Regio plume, of the Beta-Atla-Themis (BAT) region, Venus. Synthetic aperture radar data (SAR) and altimetry data from the 1989–1994 NASA Magellan mission were used to produce a geological map and history of Theia Mons, revealing two distinct magmatic centers (200 km apart), each the focus of basaltic lava flows, extensional lineaments (representing the surface expression of dyke swarms), and associated rift zones. The study area spans 88°W to 72°W, 16°45′N to 29°45′N, and mapping was at 1:500,000 scale. Our detailed mapping makes this area a prime target for the future Venus missions (orbital and lander), also given that Beta Regio is a strong candidate for ongoing volcanic activity.
Lava (basaltic) flow units (88 distinguished on the basis of variation in radar backscatter) belonging to Theia Mons volcano were combined into 19 Flow Groups and then into 3 Flow Packages. The lava flows appear to diverge from two distinct magmatic centers, labelled Center 1 (24.5°N, 78.1°W) and Center 2 (23.4° N, 79.4°W), with the older Center 1 being obscured by the volcanism of the younger Center 2. Center 1 consists of flows with low radar brightness and which extend to a maximum to 830 km from the center. Center 2 coincides with the currently preserved central caldera and consists of lava flows of low radar brightness with a maximum length of 620 km, followed by a second pulse of radar-bright flows that are less extensive and concentrated near the center.
About 10,000 extensional lineaments (grabens, fissures, and fractures) were mapped and grouped into 19 systems, of which 15 are interpreted to overlie dyke swarms: 2 radiating systems are associated with Centers 1 and 2, and 13 other systems belong to other (older and likely unrelated) magmatic centers in the region. A partial circumferential swarm may also be present, associated with Center 2.
Four other extensional lineaments sets are inferred to represent sets of normal faults associated with rift zones (Devana and Zverine, and additional rift zones). These rift zones exhibit two sets of ‘triple junction’ geometry, which are approximately also focussed on the same Centers 1 and 2, revealed by the lava flows and rift zones.
An underlying mantle plume is interpreted to be responsible for the dykes, flows and triple junction rifting. The cause of the shift between Centers 1 and 2 (200 km to SW) is unknown, but plausible mechanisms include a shift of the lithospheric plate above a stationary single plume, or a bending of the mantle plume (e.g. in a mantle wind) between timing of Center 1 and Center 2 activity.
{"title":"Geological history of Theia Mons, Beta Regio plume, Venus: Recognition of two main magmatic centers for flows, radiating dyke swarms and triple junction rifting","authors":"A.S. Shimolina , R.E. Ernst , H. El Bilali , D.G. Malyshev , V.E. Rozhin , E.G. Antropova","doi":"10.1016/j.pss.2025.106050","DOIUrl":"10.1016/j.pss.2025.106050","url":null,"abstract":"<div><div>Theia Mons (centered at 23.4° N, 79.4° W) is the main volcanic center for the Beta Regio plume, of the Beta-Atla-Themis (BAT) region, Venus. Synthetic aperture radar data (SAR) and altimetry data from the 1989–1994 NASA Magellan mission were used to produce a geological map and history of Theia Mons, revealing two distinct magmatic centers (200 km apart), each the focus of basaltic lava flows, extensional lineaments (representing the surface expression of dyke swarms), and associated rift zones. The study area spans 88°W to 72°W, 16°45′N to 29°45′N, and mapping was at 1:500,000 scale. Our detailed mapping makes this area a prime target for the future Venus missions (orbital and lander), also given that Beta Regio is a strong candidate for ongoing volcanic activity.</div><div>Lava (basaltic) flow units (88 distinguished on the basis of variation in radar backscatter) belonging to Theia Mons volcano were combined into 19 Flow Groups and then into 3 Flow Packages. The lava flows appear to diverge from two distinct magmatic centers, labelled Center 1 (24.5°N, 78.1°W) and Center 2 (23.4° N, 79.4°W), with the older Center 1 being obscured by the volcanism of the younger Center 2. Center 1 consists of flows with low radar brightness and which extend to a maximum to 830 km from the center. Center 2 coincides with the currently preserved central caldera and consists of lava flows of low radar brightness with a maximum length of 620 km, followed by a second pulse of radar-bright flows that are less extensive and concentrated near the center.</div><div>About 10,000 extensional lineaments (grabens, fissures, and fractures) were mapped and grouped into 19 systems, of which 15 are interpreted to overlie dyke swarms: 2 radiating systems are associated with Centers 1 and 2, and 13 other systems belong to other (older and likely unrelated) magmatic centers in the region. A partial circumferential swarm may also be present, associated with Center 2.</div><div>Four other extensional lineaments sets are inferred to represent sets of normal faults associated with rift zones (Devana and Zverine, and additional rift zones). These rift zones exhibit two sets of ‘triple junction’ geometry, which are approximately also focussed on the same Centers 1 and 2, revealed by the lava flows and rift zones.</div><div>An underlying mantle plume is interpreted to be responsible for the dykes, flows and triple junction rifting. The cause of the shift between Centers 1 and 2 (200 km to SW) is unknown, but plausible mechanisms include a shift of the lithospheric plate above a stationary single plume, or a bending of the mantle plume (e.g. in a mantle wind) between timing of Center 1 and Center 2 activity.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106050"},"PeriodicalIF":1.8,"publicationDate":"2025-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284621","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-01Epub Date: 2025-01-24DOI: 10.1016/j.pss.2025.106054
Suresh Sunuwar, Carlos E. Manzanares
The discovery of chlorobenzene detected in soil samples obtained in Mars has been the subject of several interpretations. The original sample was subjected to pyrolysis before the gas chromatography-mass spectrometry (GC-MS) separation and identification with the Sample Analysis at Mars (SAM) instrument on the Curiosity rover. It is believed that chlorobenzene detected at concentrations above the background level of the instrument was a product of other organic molecules reacting with perchlorates of the Martian soil. Mars surface temperatures may reach a high of about 293 K at noon, at the equator, and a low of about 120 K at the poles. In this paper, characteristic fluorescence excitation and emission spectra are presented for chlorobenzene and the suggested precursor molecules: benzoic acid, phthalic acid, and mellitic acid in transparent hexagonal water ice solutions at temperatures between 273 K and 78 K. In addition, the liquid solution spectra at 292 K. Spectra of benzene in water ice solutions have also been included. The experimental results presented in this paper are to be compared with fluorescence experiments of Mars missions that will explore the polar regions and other regions where water ice is expected to be found. Limits of detection at part per billion by mass (ng/g) concentrations at room temperature are discussed based on our results and the literature. The application of fluorescence for low temperature studies of Mars samples is also discussed with a proposed miniature instrument with a laser source to increase the sensitivity of the detection and could be used for solid or liquid samples.
{"title":"Low temperature fluorescence excitation and emission spectra of molecules relevant to Mars: Chlorobenzene, benzoic acid, phthalic acid, mellitic acid, and benzene in water ice solutions at temperatures between 78 K and 273 K","authors":"Suresh Sunuwar, Carlos E. Manzanares","doi":"10.1016/j.pss.2025.106054","DOIUrl":"10.1016/j.pss.2025.106054","url":null,"abstract":"<div><div>The discovery of chlorobenzene detected in soil samples obtained in Mars has been the subject of several interpretations. The original sample was subjected to pyrolysis before the gas chromatography-mass spectrometry (GC-MS) separation and identification with the Sample Analysis at Mars (SAM) instrument on the Curiosity rover. It is believed that chlorobenzene detected at concentrations above the background level of the instrument was a product of other organic molecules reacting with perchlorates of the Martian soil. Mars surface temperatures may reach a high of about 293 K at noon, at the equator, and a low of about 120 K at the poles. In this paper, characteristic fluorescence excitation and emission spectra are presented for chlorobenzene and the suggested precursor molecules: benzoic acid, phthalic acid, and mellitic acid in transparent hexagonal water ice solutions at temperatures between 273 K and 78 K. In addition, the liquid solution spectra at 292 K. Spectra of benzene in water ice solutions have also been included. The experimental results presented in this paper are to be compared with fluorescence experiments of Mars missions that will explore the polar regions and other regions where water ice is expected to be found. Limits of detection at part per billion by mass (ng/g) concentrations at room temperature are discussed based on our results and the literature. The application of fluorescence for low temperature studies of Mars samples is also discussed with a proposed miniature instrument with a laser source to increase the sensitivity of the detection and could be used for solid or liquid samples.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106054"},"PeriodicalIF":1.8,"publicationDate":"2025-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284560","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-01Epub Date: 2025-01-23DOI: 10.1016/j.pss.2025.106051
F. Franchi , M. Túri , G. Lakatos , K.K. Rahul , D.V. Mifsud , G. Panieri , R. Rácz , S.T.S. Kovács , E. Furu , R. Huszánk , R.W. McCullough , Z. Juhász
Methane-rich emissions to the seafloor along the Arctic mid-oceanic ridge hold strong astrobiological significance, as they may represent analogues of putative hydrothermal vent environments on Enceladus. Although such environments on Enceladus would be ideal to sample in future astrobiological missions, this may not be possible due to technological and logistical limitations. As such, searching for biosignatures in the more readily sampled cryovolcanic plumes or Enceladus’ icy shell is preferable. In this regard, the Arctic Ocean, where the geologically active seafloor is covered by thousands of metres of salty water and sealed by an ice cap, is a unique terrestrial analogue of Enceladus. In the present study, we have sought to determine whether any geochemical biosignatures associated with methane cycling (e.g., elevated methane concentrations, carbon isotopic fractionation) can be detected in Arctic ice and seawater samples using mass spectrometric techniques similar to those likely to be included in the payloads of planned missions to Enceladus. Our results have shown that, although no unequivocal evidence of methane could be detected in our Arctic samples, the carbon isotopic composition of carbon dioxide gas and the oxygen isotopic composition of water vapour emitted from the Arctic samples could indeed be measured. Furthermore, an excess of molecular hydrogen with abundances comparable to the composition of Enceladus’ southern pole plume was possibly observed in one of the Arctic ice samples. These results have implications for detectable indirect geochemical evidence of putative ecosystems of hydrogenotrophic methanogenic life on the seafloor of Enceladus and justify future efforts at method development and refinement using apparatus similar to that likely to be included in the payloads of future missions.
{"title":"An Arctic analogue for the future exploration of possible biosignatures on Enceladus","authors":"F. Franchi , M. Túri , G. Lakatos , K.K. Rahul , D.V. Mifsud , G. Panieri , R. Rácz , S.T.S. Kovács , E. Furu , R. Huszánk , R.W. McCullough , Z. Juhász","doi":"10.1016/j.pss.2025.106051","DOIUrl":"10.1016/j.pss.2025.106051","url":null,"abstract":"<div><div>Methane-rich emissions to the seafloor along the Arctic mid-oceanic ridge hold strong astrobiological significance, as they may represent analogues of putative hydrothermal vent environments on Enceladus. Although such environments on Enceladus would be ideal to sample in future astrobiological missions, this may not be possible due to technological and logistical limitations. As such, searching for biosignatures in the more readily sampled cryovolcanic plumes or Enceladus’ icy shell is preferable. In this regard, the Arctic Ocean, where the geologically active seafloor is covered by thousands of metres of salty water and sealed by an ice cap, is a unique terrestrial analogue of Enceladus. In the present study, we have sought to determine whether any geochemical biosignatures associated with methane cycling (e.g., elevated methane concentrations, carbon isotopic fractionation) can be detected in Arctic ice and seawater samples using mass spectrometric techniques similar to those likely to be included in the payloads of planned missions to Enceladus. Our results have shown that, although no unequivocal evidence of methane could be detected in our Arctic samples, the carbon isotopic composition of carbon dioxide gas and the oxygen isotopic composition of water vapour emitted from the Arctic samples could indeed be measured. Furthermore, an excess of molecular hydrogen with abundances comparable to the composition of Enceladus’ southern pole plume was possibly observed in one of the Arctic ice samples. These results have implications for detectable indirect geochemical evidence of putative ecosystems of hydrogenotrophic methanogenic life on the seafloor of Enceladus and justify future efforts at method development and refinement using apparatus similar to that likely to be included in the payloads of future missions.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106051"},"PeriodicalIF":1.8,"publicationDate":"2025-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284622","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-01Epub Date: 2025-01-30DOI: 10.1016/j.pss.2025.106063
David A. Kring , Valentin T. Bickel , Pascal Lee , Amy L. Fagan , Jennifer L. Heldmann , Rick C. Elphic , David J. Lawrence , Timothy J. Parker , Harrison H. Schmitt
The Schrödinger impact basin provides significant geological targets for future exploration, including impact melts, multi-kilometer-long exposures of magmatic rocks from deep within the lunar crust, volcanic mare, pyroclastic ash deposits, potentially with mantle xenoliths, and a geophysical setting for examining the near-rim structure of the South Pole-Aitken mega-basin. Surveyor, Ranger, and Apollo programs confirmed that constant gardening of the lunar surface by impact cratering processes reduces the availability of outcrops, which are those key bedrock exposures that geologists on Earth use as the most reliable sources of information about planetary evolution. Lunar Reconnaissance Orbiter Camera (LROC) images of the lunar surface are providing data needed to identify bedrock exposures on the Moon, and tracked boulders leading to rock exposures, in locations suitable for future exploration. One such rocky exposure occurs within a volcanic vent within the Schrödinger impact basin. We consider six working hypotheses for its origin and conclude it likely represents a bedrock exposure of impact melt and/or impact breccia produced by the Schrödinger impact event or, alternatively, pristine lava rock associated with the vent's pyroclastic origin. While elsewhere in the basin those units are covered with regolith and younger volcanic deposits, the opening of a crater floor fracture and pyroclastic eruption of volcanic material cleared a vertical exposure through the impact or eruptive lithologies, which remain accessible for exploration today.
{"title":"Potential bedrock exposures of Schrödinger impact melt sheet and/or polymict impact breccias within a crater floor fracture system and volcanic vent","authors":"David A. Kring , Valentin T. Bickel , Pascal Lee , Amy L. Fagan , Jennifer L. Heldmann , Rick C. Elphic , David J. Lawrence , Timothy J. Parker , Harrison H. Schmitt","doi":"10.1016/j.pss.2025.106063","DOIUrl":"10.1016/j.pss.2025.106063","url":null,"abstract":"<div><div>The Schrödinger impact basin provides significant geological targets for future exploration, including impact melts, multi-kilometer-long exposures of magmatic rocks from deep within the lunar crust, volcanic mare, pyroclastic ash deposits, potentially with mantle xenoliths, and a geophysical setting for examining the near-rim structure of the South Pole-Aitken mega-basin. Surveyor, Ranger, and Apollo programs confirmed that constant gardening of the lunar surface by impact cratering processes reduces the availability of outcrops, which are those key bedrock exposures that geologists on Earth use as the most reliable sources of information about planetary evolution. Lunar Reconnaissance Orbiter Camera (LROC) images of the lunar surface are providing data needed to identify bedrock exposures on the Moon, and tracked boulders leading to rock exposures, in locations suitable for future exploration. One such rocky exposure occurs within a volcanic vent within the Schrödinger impact basin. We consider six working hypotheses for its origin and conclude it likely represents a bedrock exposure of impact melt and/or impact breccia produced by the Schrödinger impact event or, alternatively, pristine lava rock associated with the vent's pyroclastic origin. While elsewhere in the basin those units are covered with regolith and younger volcanic deposits, the opening of a crater floor fracture and pyroclastic eruption of volcanic material cleared a vertical exposure through the impact or eruptive lithologies, which remain accessible for exploration today.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106063"},"PeriodicalIF":1.8,"publicationDate":"2025-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284617","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-02-01Epub Date: 2025-01-10DOI: 10.1016/j.pss.2025.106037
Jaroslav Klokočník , Jan Kostelecký , Aleš Bezděk
Gravity strike angles are one of the gravity aspects. They are computed from global static gravity field models. They react to changes in density variation and porosity. Internal rock anisotropy and stresses can be detected by strike angles. They run parallel with the direction of weakness in the strength of the rock, e.g., the direction schistosity and/or the presence of faults or micro-fault zones. Thus, they can help to describe the underground causative body in another way than traditional gravity anomalies. We used the GRGM1200A gravity field model for the Moon to the degree and order of 600 in spherical harmonic expansion and LOLA topography. The results show that the strike angles are more frequently and more intensively aligned (combed) near the poles than in other places. The strike angles are highly combed for the Malapert A crater (the landing site of IM-1/Odyssey) as well as for the localities selected by NASA for the forthcoming Artemis missions. Our method, which has already been applied many times on diverse geological features on the Earth, provides quick and cheap remote sensing procedure, a preliminary diagnostic tool, independent of all others, in search of lunar water.
{"title":"Groundwater at the southern pole of the Moon via the gravity strike angles: IM-1 and Artemis","authors":"Jaroslav Klokočník , Jan Kostelecký , Aleš Bezděk","doi":"10.1016/j.pss.2025.106037","DOIUrl":"10.1016/j.pss.2025.106037","url":null,"abstract":"<div><div>Gravity strike angles are one of the gravity aspects. They are computed from global static gravity field models. They react to changes in density variation and porosity. Internal rock anisotropy and stresses can be detected by strike angles. They run parallel with the direction of weakness in the strength of the rock, e.g., the direction schistosity and/or the presence of faults or micro-fault zones. Thus, they can help to describe the underground causative body in another way than traditional gravity anomalies. We used the GRGM1200A gravity field model for the Moon to the degree and order of 600 in spherical harmonic expansion and LOLA topography. The results show that the strike angles are more frequently and more intensively aligned (combed) near the poles than in other places. The strike angles are highly combed for the Malapert A crater (the landing site of IM-1/Odyssey) as well as for the localities selected by NASA for the forthcoming Artemis missions. Our method, which has already been applied many times on diverse geological features on the Earth, provides quick and cheap remote sensing procedure, a preliminary diagnostic tool, independent of all others, in search of lunar water.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106037"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262625","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-02-01Epub Date: 2025-01-11DOI: 10.1016/j.pss.2025.106046
Neeraja C R , Arivazhagan S , Karthi A
The compositional, chronological, topographical, and morphological features of Mare Ingenii, an impact basin situated in the northwest part of the South Pole-Aitken basin (SPA) are cha racterized using different orbital remote sensing data. Examining the chemical characteristics, spectral signatures, age, and surface features help to elucidate the basin's formation process and its volcanic evolution. In the present study, Chandrayaan-1 Moon Minerology Mapper (Ch-1 M3) data is used to prepare Standard Band Ratio (SBR), Optical Maturity (OMAT), 1000 and 2000 nm Integrated Band Depth (IBD) color composite images to map different lithologies and mafic signatures of the basin. Chandrayaan-2 Imaging Infrared Spectrometer (Ch-2 IIRS) data is used to derive 1000 and 2000 nm IBD and result is validated with M3 derived images. Minerals like olivine, pyroxene, plagioclase, spinel, and ilmenite are identified and validated through spectral studies. The FeO wt.% map from Kaguya and the TiO₂ map from the Lunar Reconnaissance Orbiter Camera - Wide Angle Camera (LROC WAC) were used to obtain FeO and TiO₂ abundances. These were then compared with abundances derived from M3 data to validate the compositional analysis. The present study identified 19 mare units in the Ingenii basin using variations in TiO2, FeO, and IBD color composite maps. Crater Size-Frequency Distribution (CSFD) technique has been employed to obtain the age of each unit and it ranges from 3.8 to 2.3 Ga and the results well correlated with previous studies. It is thus evident that Mare Ingenii has been affected by a prolonged period of mare volcanism along with a few non-mare basaltic surfaces that have been identified, including rille-related lava flows and O'Day impact melt sheets. The basin was flooded mainly by low to very low Ti basalts of the Imbrian period and patches of intermediate Ti basaltic emplacement happened during the Eratosthenian period. The topography of the basin is delineated by using Lunar Orbiter Laser Altimeter (LOLA) data and an outer ring of 600 km is mapped in this study. Morphological features such as rille, wrinkle ridge, graben, swirls, O'Day impact melt, and V-shaped features are identified using Kaguya Terrain Camera (TC) and LROC data which can offer understanding into the basin's past volcanic and cratering process. The results suggest that Mare Ingenii possesses a prolonged volcanic history and the mare is dominated by low to very low Ti basalts sourced from olivine-ilmenite-pyroxene cumulates.
{"title":"Lunar Mare Ingenii: A comprehensive multi data study unravelling composition, chronology and terrain dynamics","authors":"Neeraja C R , Arivazhagan S , Karthi A","doi":"10.1016/j.pss.2025.106046","DOIUrl":"10.1016/j.pss.2025.106046","url":null,"abstract":"<div><div>The compositional, chronological, topographical, and morphological features of Mare Ingenii, an impact basin situated in the northwest part of the South Pole-Aitken basin (SPA) are cha racterized using different orbital remote sensing data. Examining the chemical characteristics, spectral signatures, age, and surface features help to elucidate the basin's formation process and its volcanic evolution. In the present study, Chandrayaan-1 Moon Minerology Mapper (Ch-1 M<sup>3</sup>) data is used to prepare Standard Band Ratio (SBR), Optical Maturity (OMAT), 1000 and 2000 nm Integrated Band Depth (IBD) color composite images to map different lithologies and mafic signatures of the basin. Chandrayaan-2 Imaging Infrared Spectrometer (Ch-2 IIRS) data is used to derive 1000 and 2000 nm IBD and result is validated with M<sup>3</sup> derived images. Minerals like olivine, pyroxene, plagioclase, spinel, and ilmenite are identified and validated through spectral studies. The FeO wt.% map from Kaguya and the TiO₂ map from the Lunar Reconnaissance Orbiter Camera - Wide Angle Camera (LROC WAC) were used to obtain FeO and TiO₂ abundances. These were then compared with abundances derived from M<sup>3</sup> data to validate the compositional analysis. The present study identified 19 mare units in the Ingenii basin using variations in TiO<sub>2</sub>, FeO, and IBD color composite maps. Crater Size-Frequency Distribution (CSFD) technique has been employed to obtain the age of each unit and it ranges from 3.8 to 2.3 Ga and the results well correlated with previous studies. It is thus evident that Mare Ingenii has been affected by a prolonged period of mare volcanism along with a few non-mare basaltic surfaces that have been identified, including rille-related lava flows and O'Day impact melt sheets. The basin was flooded mainly by low to very low Ti basalts of the Imbrian period and patches of intermediate Ti basaltic emplacement happened during the Eratosthenian period. The topography of the basin is delineated by using Lunar Orbiter Laser Altimeter (LOLA) data and an outer ring of 600 km is mapped in this study. Morphological features such as rille, wrinkle ridge, graben, swirls, O'Day impact melt, and V-shaped features are identified using Kaguya Terrain Camera (TC) and LROC data which can offer understanding into the basin's past volcanic and cratering process. The results suggest that Mare Ingenii possesses a prolonged volcanic history and the mare is dominated by low to very low Ti basalts sourced from olivine-ilmenite-pyroxene cumulates.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106046"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262395","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-02-01Epub Date: 2025-01-08DOI: 10.1016/j.pss.2025.106036
Gaëlle Belleau-Magnat , Myriam Lemelin , Edward Cloutis , Richard Léveillé
Gossans are formed through the oxidation of sulfide ore deposits by fluids, such as meteoric water or hydrothermal solutions, leading to locally acidic conditions. In permafrost regions, gossans undergo seasonal chemical weathering after their initial formation (reactive gossans), potentially providing a sustained energy source for microbial activity. Arctic gossans are therefore considered valuable analogs for Martian paleo-hydrothermal systems and promising astrobiological targets. While hundreds of gossans have been identified in the Arctic, few have been studied in detail and even fewer using rover-compatible remote sensing techniques. This study aims to characterize the morphological profile of seven Arctic gossans located at Expedition Fiord (Axel Heiberg Island, Nunavut), as well as their geochemistry, mineralogy and organic carbon content using X-ray fluorescence, X-ray diffraction (XRD), Visible (VNIR) to thermal infrared (MIR-TIR) reflectance and Raman spectroscopy. Results showed a dominance of silicon, calcium and iron. Mineralogical analyses revealed gypsum and quartz as major phases, with variable amounts of silicates, sulfates, iron sulfides and iron oxyhydroxides. Raman spectroscopy detected organic carbon in most samples, up to 50 cm deep, in various organo-mineral complexes. XRD was the only technique to detect iron sulfides. VNIR-MIR-TIR reflectance and Raman spectroscopy provided mineralogical results consistent with XRD. All gossans displayed classical profiles, with alteration zones overlying primary sulfides, but showed diverse color and compositional stratification patterns. These variations suggest local mechanisms influence mineral and associated organic carbon distribution. Further investigations should focus on better understanding these local variations, which could guide the search for biosignatures in gossan-like features on Mars.
Gossans是通过流体（如大气水或热液溶液）氧化硫化物矿床形成的，导致局部酸性条件。在永久冻土区，蛛丝在初始形成后经历季节性化学风化（活性蛛丝），可能为微生物活动提供持续的能量来源。因此，北极蛛丝被认为是火星古热液系统和有前途的天体生物学目标的有价值的类似物。虽然在北极已经发现了数百种蛛丝，但对它们进行详细研究的很少，使用与漫游车兼容的遥感技术的就更少了。本研究旨在利用x射线荧光、x射线衍射（XRD）、可见(VNIR) -热红外（MIR-TIR）反射率和拉曼光谱，表征位于努纳武特探险峡湾（Axel Heiberg Island, Nunavut）的7种北极蛛的形态特征，以及它们的地球化学、矿物学和有机碳含量。结果表明，硅、钙和铁占主导地位。矿物学分析显示，石膏和石英为主要相，硅酸盐、硫酸盐、硫化铁和氧化铁含量不等。拉曼光谱在大多数样品中检测到有机碳，深度可达50厘米，在各种有机矿物复合物中。XRD是检测硫化铁的唯一方法。VNIR-MIR-TIR反射率和拉曼光谱的矿物学结果与XRD一致。所有丝织物均表现出典型的剖面，蚀变带位于原生硫化物之上，但颜色和成分分层模式各异。这些变化表明局部机制影响矿物和相关有机碳分布。进一步的研究应该集中在更好地理解这些局部变化上，这可以指导在火星上寻找类似戈桑的生物特征。
{"title":"Mineralogy, geochemistry and morphology of Arctic gossans on Axel Heiberg Island, NU, Canada: Spectroscopic investigation and implications for Mars","authors":"Gaëlle Belleau-Magnat , Myriam Lemelin , Edward Cloutis , Richard Léveillé","doi":"10.1016/j.pss.2025.106036","DOIUrl":"10.1016/j.pss.2025.106036","url":null,"abstract":"<div><div>Gossans are formed through the oxidation of sulfide ore deposits by fluids, such as meteoric water or hydrothermal solutions, leading to locally acidic conditions. In permafrost regions, gossans undergo seasonal chemical weathering after their initial formation (reactive gossans), potentially providing a sustained energy source for microbial activity. Arctic gossans are therefore considered valuable analogs for Martian paleo-hydrothermal systems and promising astrobiological targets. While hundreds of gossans have been identified in the Arctic, few have been studied in detail and even fewer using rover-compatible remote sensing techniques. This study aims to characterize the morphological profile of seven Arctic gossans located at Expedition Fiord (Axel Heiberg Island, Nunavut), as well as their geochemistry, mineralogy and organic carbon content using X-ray fluorescence, X-ray diffraction (XRD), Visible (VNIR) to thermal infrared (MIR-TIR) reflectance and Raman spectroscopy. Results showed a dominance of silicon, calcium and iron. Mineralogical analyses revealed gypsum and quartz as major phases, with variable amounts of silicates, sulfates, iron sulfides and iron oxyhydroxides. Raman spectroscopy detected organic carbon in most samples, up to 50 cm deep, in various organo-mineral complexes. XRD was the only technique to detect iron sulfides. VNIR-MIR-TIR reflectance and Raman spectroscopy provided mineralogical results consistent with XRD. All gossans displayed classical profiles, with alteration zones overlying primary sulfides, but showed diverse color and compositional stratification patterns. These variations suggest local mechanisms influence mineral and associated organic carbon distribution. Further investigations should focus on better understanding these local variations, which could guide the search for biosignatures in gossan-like features on Mars.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106036"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262393","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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