Journal of Geophysical Research: Planets最新文献_第5页

Water-Limited Hydrothermalism and Volcanic Resurfacing of Eridania Basin, Mars 火星埃里达尼亚盆地的限水热液作用和火山重铺

IF 3.9 1区地球科学

Journal of Geophysical Research: Planets Pub Date : 2024-07-11 DOI: 10.1029/2024JE008461

Emmy B. Hughes, James Wray, Suniti Karunatillake, Grace Fanson, Elise Harrington, Don R. Hood

{"title":"Water-Limited Hydrothermalism and Volcanic Resurfacing of Eridania Basin, Mars","authors":"Emmy B. Hughes, James Wray, Suniti Karunatillake, Grace Fanson, Elise Harrington, Don R. Hood","doi":"10.1029/2024JE008461","DOIUrl":"https://doi.org/10.1029/2024JE008461","url":null,"abstract":"The Eridania Basin system, located in the martian southern highlands, may have hosted long-lived lacustrine hydrothermalism. Despite its multi-basin scale and suggested longevity that should pervasively alter the landscape, evidence for consistent compositional signatures of lacustrine hydrothermalism across varying spatial scales is poorly known. Here we synthesize orbital data sets (derived from the Gamma Ray Spectrometer, GRS; Thermal Emission Spectrometer, TES; and Compact Reconnaissance Imaging Spectrometer for Mars, CRISM) to characterize the composition of Eridania's landscape from regional to outcrop scales. The bulk geochemistry representing decimeter depths is broadly on par with mafic igneous compositions seen elsewhere on Mars. The landscape-scale mineralogy of Eridania suggests a compositional distinction between Eridania's northernmost basin and the remaining basins. Meanwhile, chloride mapping and analyses of amorphous silica and acid-altered clay phases at the outcrop scale both show that mineralogical evidence for hydrothermal alteration and putative lacustrine activity is broadly limited to the northernmost basin, and that most other amorphous silica in Eridania is consistent with low-to-minimal water/rock weathering. This suggests either limited regional hydrothermalism or extensive mafic resurfacing occurred in Eridania, the latter of which is consistent with previous studies. Our findings collectively suggest that Eridania underwent local crystal hydrothermal alteration, perhaps confined to the northernmost basin, while much of the remainder of the Eridania's basins either experienced low-temperature weathering or extensive resurfacing to at least meter scale depths by later volcanism. This supports prior inferences of spatially and temporally limited surface hydrology on Mars and extensive volcanic resurfacing of basins, as in the Gusev Crater.","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":null,"pages":null},"PeriodicalIF":3.9,"publicationDate":"2024-07-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008461","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141597151","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}

引用次数: 0

Dayside Magnetodisk Reconnection in Jovian System: Galileo and Voyager Observation 彗星系统中的日侧磁盘再连接：伽利略和旅行者观测

IF 3.9 1区地球科学

Journal of Geophysical Research: Planets Pub Date : 2024-07-11 DOI: 10.1029/2023JE008240

Jinyan Zhao, Ruilong Guo, Quanqi Shi, Tao Tang, Alexander William Degeling, Zhonghua Yao, Denis Grodent, Shi-Chen Bai, Jong-Sun Park, Xiao Ma, Junjie Chen, Binzheng Zhang, Huizi Wang, Anmin Tian, Qiugang Zong

{"title":"Dayside Magnetodisk Reconnection in Jovian System: Galileo and Voyager Observation","authors":"Jinyan Zhao, Ruilong Guo, Quanqi Shi, Tao Tang, Alexander William Degeling, Zhonghua Yao, Denis Grodent, Shi-Chen Bai, Jong-Sun Park, Xiao Ma, Junjie Chen, Binzheng Zhang, Huizi Wang, Anmin Tian, Qiugang Zong","doi":"10.1029/2023JE008240","DOIUrl":"https://doi.org/10.1029/2023JE008240","url":null,"abstract":"Magnetic reconnection, an essential mechanism in plasma physics that changes magnetic topology and energizes charged particles, plays a vital role in the dynamic processes of the Jovian magnetosphere. The traditional Vasyliūnas cycle only considers the effect of magnetic reconnection at the nightside magnetodisk. Recently, magnetic reconnection has been identified at the dayside magnetodisk in Saturn's magnetosphere and can impact dayside auroral processes. In this study, we provide the first evidence that the dayside magnetodisk reconnection can also occur at Jupiter. Using data from the Galileo and Voyager 2 spacecraft, we have identified 18 dayside reconnection events with radial distances in the range of 30–60 Jupiter radii (RJ). We analyzed the particle (electron and ion) flux, energy spectra, and characteristic energy of these dayside events and compared them to the nightside events. The statistical results show that the energy spectra and characteristic energy of electrons/ions in dayside and nightside magnetic reconnection events are comparable. On average, the characteristic energy of ions on the dayside is higher than that on the nightside. Based on the limited data set, we speculate that the occurrence rate of dayside magnetodisk reconnection should be significant. The dayside Jovian magnetodisk reconnection seems to have a comparable effect on providing energetic particles as that at nightside and to be one of the key processes driving dynamics within the Jovian magnetosphere.","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":null,"pages":null},"PeriodicalIF":3.9,"publicationDate":"2024-07-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008240","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141597147","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}

引用次数: 0

Modeling of the Impact-Generated Hydrothermal System at the Haughton Impact Structure 霍顿撞击结构的撞击生成热液系统建模

IF 3.9 1区地球科学

Journal of Geophysical Research: Planets Pub Date : 2024-07-10 DOI: 10.1029/2023JE008267

A. J. Trowbridge, Simone Marchi, Gordon R. Osinski, Joshua M. Taron

{"title":"Modeling of the Impact-Generated Hydrothermal System at the Haughton Impact Structure","authors":"A. J. Trowbridge, Simone Marchi, Gordon R. Osinski, Joshua M. Taron","doi":"10.1029/2023JE008267","DOIUrl":"https://doi.org/10.1029/2023JE008267","url":null,"abstract":"Hypervelocity impacts can generate hydrothermal systems, which have been suggested as candidate environments for prebiotic chemistry on the early Earth. The Haughton impact structure (a 23 km diameter crater located on Devon Island, Nunavut, Arctic Canada) displays evidence of water-rock alteration indicative of a hydrothermal system generated from a cosmic impact. To model the formation of this crater and subsequent hydrothermal alteration, we have successfully developed a new two-code methodology that utilizes a shock physics code and a hydrothermal code (HYDROTHERM). We can best reproduce the Haughton crater with a ∼700 m diameter projectile with an impact velocity of 14 km/s. With our approach, we were able to match all the major geological constraints observed at the Haughton impact structure. Our models show that the Haughton crater interior could have sustained temperatures ideal for thermophilic and hyperthermophilic life (50–120°C) for more than 50,000 years, indicating that these systems can sustain prebiotic chemistry and life for longer than previously estimated.","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":null,"pages":null},"PeriodicalIF":3.9,"publicationDate":"2024-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141584108","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}

引用次数: 0

The Venus Global Ionosphere-Thermosphere Model (V-GITM): A Coupled Thermosphere and Ionosphere Formulation 金星全球电离层-热层模型（V-GITM）：热层和电离层耦合模型

IF 3.9 1区地球科学

Journal of Geophysical Research: Planets Pub Date : 2024-07-10 DOI: 10.1029/2023JE008079

Brandon M. Ponder, Aaron J. Ridley, Stephen W. Bougher, David Pawlowski, Amanda Brecht

{"title":"The Venus Global Ionosphere-Thermosphere Model (V-GITM): A Coupled Thermosphere and Ionosphere Formulation","authors":"Brandon M. Ponder, Aaron J. Ridley, Stephen W. Bougher, David Pawlowski, Amanda Brecht","doi":"10.1029/2023JE008079","DOIUrl":"https://doi.org/10.1029/2023JE008079","url":null,"abstract":"This paper introduces the new Venus global ionosphere-thermosphere model (V-GITM) which incorporates the terrestrial GITM framework with Venus-specific parameters, ion-neutral chemistry, and radiative processes in order to simulate some of the observable features regarding the temperatures, composition, and dynamical structure of the Venus atmosphere from 70 to 170 km. Atmospheric processes are included based upon formulations used in previous Venus GCMs, several augmentations exist, such as improved horizontal and vertical momentum equations and tracking exothermic chemistry. Explicitly solving the momentum equations allows for the exploration of its dynamical effects on the day-night structure. In addition, V-GITM's use of exothermic chemistry instead of a strong heating efficiency accounts for the heating due to the solar EUV while producing comparable temperatures to empirical models. V-GITM neutral temperatures and neutral-ion densities are compared to upper atmosphere measurements obtained from Pioneer Venus and Venus Express. V-GITM demonstrates asymmetric horizontal wind velocities through the cloud tops to the middle thermosphere and explains the mechanisms for sustaining the wind structure. In addition, V-GITM produces reasonable dayside ion densities and shows that the neutral winds can carry the ions to the nightside via an experiment advecting <math>\u0000 <semantics>\u0000 <mrow>\u0000 <msubsup>\u0000 <mi>O</mi>\u0000 <mn>2</mn>\u0000 <mo>+</mo>\u0000 </msubsup>\u0000 </mrow>\u0000 <annotation> ${mathrm{O}}_{2}^{+}$</annotation>\u0000 </semantics></math>.","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":null,"pages":null},"PeriodicalIF":3.9,"publicationDate":"2024-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008079","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141584112","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}

引用次数: 0

Acoustic Propagation in the Near-Surface Martian Atmosphere 近地表火星大气中的声波传播

IF 3.9 1区地球科学

Journal of Geophysical Research: Planets Pub Date : 2024-07-10 DOI: 10.1029/2024JE008469

Martin Gillier, Andi Petculescu, Alexander E. Stott, Naomi Murdoch, Xavier Jacob, Baptiste Chide, Sylvestre Maurice, David Mimoun

{"title":"Acoustic Propagation in the Near-Surface Martian Atmosphere","authors":"Martin Gillier, Andi Petculescu, Alexander E. Stott, Naomi Murdoch, Xavier Jacob, Baptiste Chide, Sylvestre Maurice, David Mimoun","doi":"10.1029/2024JE008469","DOIUrl":"https://doi.org/10.1029/2024JE008469","url":null,"abstract":"This work introduces a comprehensive model of sound propagation on Mars, in light of the recent operation of several microphones on the Martian surface. The main outcome of this work is an operational acoustic model capable of simulating the sound field created by any source, at any location on the Martian surface, at any time. Expanding on the result of previous work (Gillier et al., 2024, https://doi.org/10.1029/2023je008257), we use the parabolic equation method for sound propagation in order to obtain the overall sound field produced by a source, in a given atmospheric composition and state, and accounting for ground properties. The resulting model enables the study of acoustics on Mars, and has the potential also to be used to probe the properties of the Martian environment using acoustic measurements with known sources. We investigate the effects of the Martian ground and the vertical profile of temperature and wind, on sound propagation. We find that the ground has a minor effect on sound propagation, and the wind profile strongly influences sound propagation as on Earth. However, the midday near surface temperature profiles on Mars are shown to cause refraction, which generates non-negligible acoustic losses that are an order of magnitude stronger than typical refraction-related acoustic losses on Earth. We show that the effect of the Martian atmospheric turbulence is to slightly reduce the acoustic losses due to refraction. Finally, we apply our model to show that refraction and atmospheric turbulence have a negligible effect on the propagation of sound from Ingenuity to the Perseverance rover.","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":null,"pages":null},"PeriodicalIF":3.9,"publicationDate":"2024-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008469","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141584111","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}

引用次数: 0

The Role and Lifetime of Dissociative Heterogeneous Processes in Improving Simulated Ozone on Mars 分解异质过程在改善火星模拟臭氧中的作用和寿命

IF 3.9 1区地球科学

Journal of Geophysical Research: Planets Pub Date : 2024-07-09 DOI: 10.1029/2024JE008302

M. A. J. Brown, M. R. Patel, S. R. Lewis, J. A. Holmes, F. Lefèvre, J. P. Mason, M. Crismani

{"title":"The Role and Lifetime of Dissociative Heterogeneous Processes in Improving Simulated Ozone on Mars","authors":"M. A. J. Brown, M. R. Patel, S. R. Lewis, J. A. Holmes, F. Lefèvre, J. P. Mason, M. Crismani","doi":"10.1029/2024JE008302","DOIUrl":"https://doi.org/10.1029/2024JE008302","url":null,"abstract":"Ozone simulated in Mars Global Climate Models (MGCMs) is used to assess the underlying chemistry occurring in the atmosphere. Currently, ozone total column abundance (TCA) is under-predicted in MGCMs by up to 120%, implying missing or inaccurate chemistry in models. Heterogeneous reactions of hydroxyl radicals (HOX) have been offered as an explanation for some of this bias, because they cause ozone to increase at locations where it's currently under-predicted. We use four simulations to compare modeled ozone TCA with observations from the UVIS spectrometer aboard the ExoMars Trace Gas Orbiter to improve the representation of heterogeneous processes and their impact on ozone. We use a gas-phase only run, a dissociative scheme, an adsorbed HOX retention scheme, and a hybrid scheme that combines the dissociative mechanism with the retention of HOX on water ice. We find retention of HOX is dependent on water ice sublimation, and ozone abundance increases when water ice persists for longer periods (1–20 sols). Over time, the loss of HOX causes a depletion in H2O2 concentration (HOX reservoir), and thus allows ozone concentration to increase. When adsorbed HOX are desorbed and dissociate into other by-products, HOX are not immediately available to destroy ozone. This results in larger ozone concentrations than if desorbed HOX are released directly back into their gaseous states. When using the hybrid scheme, ozone TCA is increased up to 50% where the ozone deficit is greatest, demonstrating the best agreement with observations, and implying that HOX radicals are both retained when adsorbed and dissociate.","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":null,"pages":null},"PeriodicalIF":3.9,"publicationDate":"2024-07-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008302","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141583731","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}

引用次数: 0

Topography-Enhanced Ultra-Cold Trapping at the LCROSS Impact Site LCROSS撞击点的地形增强型超冷捕获

IF 3.9 1区地球科学

Journal of Geophysical Research: Planets Pub Date : 2024-07-09 DOI: 10.1029/2023JE007925

C. W. Hayes, D. A. Minton, J. L. Kloos, J. E. Moores

{"title":"Topography-Enhanced Ultra-Cold Trapping at the LCROSS Impact Site","authors":"C. W. Hayes, D. A. Minton, J. L. Kloos, J. E. Moores","doi":"10.1029/2023JE007925","DOIUrl":"https://doi.org/10.1029/2023JE007925","url":null,"abstract":"Small topographic features below the resolution of existing orbital data sets may create “micro ultra-cold traps” within the larger permanently shadowed regions that are present at the lunar poles. These ultra-cold traps are protected from the major primary and secondary illumination sources, and thus would create surfaces that are much colder than lower-resolution temperature maps would indicate. We examine this effect by creating a high resolution (1 m pix−1) terrain map based on upscaled data from the Lunar Orbiter Laser Altimeter. This map is illuminated by scattered sunlight and infrared emissions from sunlit terrain, which are then run through a thermal model to determine temperatures. We find that while most of the terrain experiences maximum temperatures around 50 K, there are a number of 1–30 m-scale ultra-cold traps with maximum temperatures as low as 20–30 K. By comparing our modeled ultra-cold trapping area to volatile abundances measured by Lunar Crater Observation and Sensing Satellite (LCROSS), we reveal a diverse environment where the surficial abundances necessary to explain the LCROSS results are strongly dependent on precisely where the impact occurred.","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":null,"pages":null},"PeriodicalIF":3.9,"publicationDate":"2024-07-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE007925","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141583730","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}

引用次数: 0

Mechanical Properties of LL6 Chondrites Under Pressures Relevant to Rocky Interiors of Icy Moons 冰卫星岩石内部相关压力下的 LL6 颗软玉的力学特性

IF 3.9 1区地球科学

Journal of Geophysical Research: Planets Pub Date : 2024-07-08 DOI: 10.1029/2024JE008296

Cassandra Seltzer, Hoagy O'Ghaffari, Matěj Peč

{"title":"Mechanical Properties of LL6 Chondrites Under Pressures Relevant to Rocky Interiors of Icy Moons","authors":"Cassandra Seltzer, Hoagy O'Ghaffari, Matěj Peč","doi":"10.1029/2024JE008296","DOIUrl":"https://doi.org/10.1029/2024JE008296","url":null,"abstract":"Icy moons in the outer Solar System likely contain rocky, chondritic interiors, but this material is rarely studied under confining pressure. The contribution of rocky interiors to deformation and heat generation is therefore poorly constrained. We deformed LL6 chondrites at confining pressures ≤100 MPa and quasistatic strain rates. We defined a failure envelope, recorded acoustic emissions (AEs), measured ultrasonic velocities, and retrieved static and dynamic elastic moduli for the experimental conditions. The Young's modulus, which quantifies stiffness, of the chondritic material increased with increasing confining pressure. The material reached its peak strength, which is the maximum supported differential stress (σ1 − σ3), between 40 and 50 MPa confining pressure. Above this 40–50 MPa range of confining pressure, the stiffness increased significantly, while the peak strength dropped. Acoustic emission events associated with brittle deformation mechanisms occurred both during isotropic pressurization (σ1 = σ2 = σ3) as well as at low differential stresses during triaxial deformation (σ1 > σ2 = σ3), during nominally “elastic” deformation, indicating that dissipative processes are likely possible in the rocky interiors of icy moons. These events also occurred less frequently at higher confining pressures. We therefore suggest that the chondritic interiors of icy moons could become less compliant, and possibly less dissipative, as a function of the moons' pressure and size.","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":null,"pages":null},"PeriodicalIF":3.9,"publicationDate":"2024-07-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008296","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141565871","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}

引用次数: 0

New Views of Lunar Seismicity Brought by Analysis of Newly Discovered Moonquakes in Apollo Short-Period Seismic Data 分析阿波罗短周期地震数据中新发现的月震带来的月球地震新观点

IF 3.9 1区地球科学

Journal of Geophysical Research: Planets Pub Date : 2024-07-05 DOI: 10.1029/2023JE008153

Keisuke Onodera

{"title":"New Views of Lunar Seismicity Brought by Analysis of Newly Discovered Moonquakes in Apollo Short-Period Seismic Data","authors":"Keisuke Onodera","doi":"10.1029/2023JE008153","DOIUrl":"https://doi.org/10.1029/2023JE008153","url":null,"abstract":"In the 1970s, two types of seismometers were installed on the nearside of the Moon. One type is called the Long-Period (LP) seismometer, which is sensitive below 1.5 Hz. The other is called the Short-Period (SP) seismometer, whose sensitivity is high around 2–10 Hz. So far, more than 13,000 seismic events have been identified through analyzing the LP data, which allowed us to investigate lunar seismicity and its internal structure. On the other hand, most of the SP data have remained unanalyzed because they include numerous artifacts. This fact leads to the hypotheses that (a) we have missed lots of high-frequency seismic events and (b) lunar seismicity could be underestimated. To verify these ideas, I conducted an analysis of the SP data. In the analysis, I denoised the original SP data and performed the event detections by comparing the spectral features between the cataloged high-frequency events (such as shallow moonquakes) and the continuous SP data. Eventually, I discovered 22,000 new seismic events, including thermal moonquakes, impact-induced events, and shallow moonquakes. Among these, I focused on analyzing shallow moonquakes—tectonic-related quakes. Consequently, it turned out that there were 2.6 times more tectonic events than considered before. Furthermore, additional detections of shallow moonquakes enabled me to see the regionality in seismicity. Comparing three landing sites (Apollo 14, 15, and 16), I found that the Apollo 15 site was more seismically active than others. These findings can change the conventional views of lunar seismicity.","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":null,"pages":null},"PeriodicalIF":3.9,"publicationDate":"2024-07-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008153","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141536582","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}

引用次数: 0

Amazonian Tectonic Evolution of Ceraunius and Tractus Fossae, Mars, and Implications for Local Magmatic Sources 火星 Ceraunius 和 Tractus Fossae 的亚马逊构造演化及其对当地岩浆源的影响

IF 3.9 1区地球科学

Journal of Geophysical Research: Planets Pub Date : 2024-07-04 DOI: 10.1029/2023JE008123

Stephanie Shahrzad, Emma K. Bramham, Sandra Piazolo, Mark Thomas, Paul K. Byrne

{"title":"Amazonian Tectonic Evolution of Ceraunius and Tractus Fossae, Mars, and Implications for Local Magmatic Sources","authors":"Stephanie Shahrzad, Emma K. Bramham, Sandra Piazolo, Mark Thomas, Paul K. Byrne","doi":"10.1029/2023JE008123","DOIUrl":"https://doi.org/10.1029/2023JE008123","url":null,"abstract":"The heavily faulted Martian terrains of Ceraunius Fossae and Tractus Fossae, south of the Alba Mons volcano, have previously only been considered as parts of larger tectonic studies of Alba Mons, and consequently the complexity of the faulting remains unclear. As these terrains are in the midst of the large Tharsis volcanoes, the study of their surface deformation has the potential to help unravel the volcano-tectonic deformation associated with the growth of Tharsis as well as to decipher details of the magma-tectonic processes responsible for graben formation. Here, we distinguish between faults and collapse structures based on image and topographic evidence. We mapped ∼12,000 faults, which we grouped into three distinct fault groups based on orientation, morphology, and relative ages. These show a temporal evolution in the mapped fault orientations from NE to N-S to NW with associated changes in stress orientations. We also mapped collapse features and categorized them into four different groups: pit-crater chains, catenae, u-shaped troughs and chasmata. Examining the four collapse structure groups reveals that they are likely four progressive stages in the erosional evolution of pit-crater chains. Together, this revealed a structural history heavily influenced by lateral diking from both local (radial to Alba Mons, Pavonis Mons and Ascraeus Mons) and regional (radial to Tharsis) sources, and vertical diking from a proposed Ceraunius Fossae centered magma source. This, along with an updated crater size-frequency distribution analysis of the unit ages, reveals a highly active tectonic and magmatic environment south of Alba Mons in the Middle Amazonian.","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":null,"pages":null},"PeriodicalIF":3.9,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008123","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141536674","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}

引用次数: 0