Journal of Geophysical Research: Planets最新文献

{"title":"Thermal Evolution of Planetary Interiors With a Crystallizing Basal Magma Ocean Coupled to Parameterized Mantle Convection","authors":"Victoria Auerbach,&nbsp;Dave R. Stegman","doi":"10.1029/2025JE009016","DOIUrl":"10.1029/2025JE009016","url":null,"abstract":"<p>Basal magma oceans (BMOs) persisting in the silicate portion of terrestrial planets for long periods of time (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>&gt;</mo>\u0000 </mrow>\u0000 <annotation> ${ &gt;} $</annotation>\u0000 </semantics></math>1 Gyr) offer the potential to reconcile unexplained contradictions between geochemical and geophysical observations, yet our knowledge of how the presence of such layers influence planetary evolution is far from mature. In this study, we produce 1D thermal evolution models using parameterized convection for Earth and Venus-like planets with consideration of a long-lived BMO. In these models, we independently vary initial conditions and material properties of the system which are shown to have strong control on the thermal evolution of the system and associated crystallization rate of the BMO. We find small variations in viscosity prefactors, lower mantle activation volume, or melt depression of the liquid melting curve to have significant impact on the solid-liquid interface and temperature evolution of the system. Similarly, small variations in initial conditions produces a shift in comparable Earth and Venus models. In general, we observe the thermal boundary layer between the solid and liquid mantle layers governs the coupling of the system and therefore its evolution. These parameterized models demonstrate the capability to better understand impact of individual parameters and coupling of interior layers, which drive the thermal evolution for both Earth and Venus cases.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 7","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-07-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009016","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144687949","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":"Nighttime and Early Morning Atmospheric Waves and Transient Turbulence at Jezero Crater, Mars, Observed by the Perseverance Rover","authors":"A. Munguira,&nbsp;R. Hueso,&nbsp;A. Sánchez-Lavega,&nbsp;T. del Rio-Gaztelurrutia,&nbsp;T. Bertrand,&nbsp;G. M. Martínez","doi":"10.1029/2025JE009114","DOIUrl":"10.1029/2025JE009114","url":null,"abstract":"<p>We study atmospheric oscillations in Jezero crater, Mars, that occur at night and dawn over stable conditions of the planetary boundary layer. These atmospheric oscillations are sporadic and can have large amplitudes, resulting in important variations in the dynamic conditions of the atmosphere. We analyze simultaneous measurements of atmospheric pressure and temperature data obtained in situ by the Mars Environmental Dynamics Analyzer (MEDA) instrument onboard the Mars2020/Perseverance rover. The observations span two Martian years of data at the crater floor and in the delta. We separate the wavelike and turbulent components of the oscillations, and use spectral analysis to examine the spectral slopes associated with different types of pressure oscillations. We identify four types of atmospheric transient oscillations: gravity waves (GW), solitary wavelike pulses (SoW), a nighttime pressure dip consistent with a solitary wave of depression, and possible Kelvin-Helmholtz (K-H) waves associated with high local turbulence. We examine diurnal and seasonal trends associated with the frequency of occurrence of these events. All the oscillations are less intense and less frequent around the aphelion season. The diurnal and seasonal trends in GW and SoW are consistent with previous studies at other locations on Mars, which may support a forcing by the large-scale atmospheric circulation. Potential K-H waves were observed during periods of relatively high dust opacity and in complex terrains, suggesting an origin near the surface when compared with similar observations on Earth. These waves had periods of 3.0–11.1 min and induced high-frequency turbulence.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 7","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-07-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009114","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144673062","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":"Diurnal Cycle of Non-Orographic Gravity Waves' Source Altitudes and Its Impacts: Tests With Mars Planetary Climate Model","authors":"Jiandong Liu,&nbsp;Ehouarn Millour,&nbsp;François Forget,&nbsp;Gabriella Gilli,&nbsp;François Lott,&nbsp;Deborah Bardet,&nbsp;Francisco González Galindo","doi":"10.1029/2024JE008880","DOIUrl":"10.1029/2024JE008880","url":null,"abstract":"<p>The transfer of momentum due to non-orographic Gravity Waves (GWs) significantly regulates the Martian middle-upper atmospheric dynamics. Thus, these waves influence the transport of tracers and escape in the thermosphere. However, models assume that the non-orographic GWs are emitted from a constant source level that approximates the averaged Planetary Boundary Layer (PBL). We move on to impose that the emission of the waves follows the top of a real-time evaluated PBL to account for the diurnal cycle of the waves' source altitudes and implement this improvement in the Mars Planetary Climate Model (Mars PCM). In the absence of the PBL during the night, the non-orographic GWs are assumed to be launched at altitudes near the surface following Hinson and Wilson (2023, https://doi.org/10.1016/j.icarus.2022.115420)'s results. Sensitivity tests with the Mars PCM show that non-orographic GWs are built up efficiently during the (polar) night. With the new scheme, the angular momentum in the upper atmosphere is enhanced. Additionally, simulations recover the “cold pockets” in temperature observed by the Mars Climate Sounder at 80–100 km and capture “deep drops” of the atmospheric species recorded by the Neutral Gas and Ion Mass Spectrometer in the polar night.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 7","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-07-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008880","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144673174","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":"Small in Number but Mighty in Significance: Impact Craters as Windows Into Europa's Subsurface","authors":"Jennifer E. C. Scully,&nbsp;Michael J. Malaska,&nbsp;Erin J. Leonard,&nbsp;Marissa E. Cameron,&nbsp;Heather A. Lethcoe,&nbsp;Cynthia B. Phillips,&nbsp;Richard J. Cartwright,&nbsp;Elodie Lesage,&nbsp;Mohit Melwani Daswani,&nbsp;Lauren E. McKeown","doi":"10.1029/2024JE008670","DOIUrl":"10.1029/2024JE008670","url":null,"abstract":"<p>Impact craters are rare on the icy ocean world Europa: only 24 ≧ 10 km in diameter are currently observed. Craters ≳20 km in diameter, such as Pwyll and Manannán, display unusual morphologies, perhaps because they excavate down close to the subsurface ocean. Previous work suggests that Manannán may have impacted into liquid, slushy ice or thinner ice than at Pwyll. Here we show that impact craters, via their intrinsic morphologic and compositional properties, as well as impact-excavation of otherwise unobservable materials, provide windows into subsurface structure and composition, making them natural laboratories for investigating Europa's habitability. We find that both Pwyll and Manannán excavated dark material from ∼3.1 km deep, which could be intriguing non-ice materials such as H₂SO₄ or hydrated minerals. We calculated that Pwyll impacted into a solid ice shell of ≧10.7 km thickness. We hypothesize that Manannán may have impacted into less viscous material, and detail how this can be tested with future Europa Clipper data. We also hypothesize that a reservoir of sub-surface impact-induced material sourced the lobate material within Pwyll. This hypothesis can also be tested with Europa Clipper data and, if confirmed, would provide targets to observe salts derived from potentially some of the most processed brines on Europa.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 7","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-07-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144666466","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":"Formation of Martian Wrinkle Ridges: New Insights From Analog Experiments on Décollement Processes","authors":"Zheren Zhao,&nbsp;Shichao Li,&nbsp;Chuang Sun,&nbsp;Hongtao Wang,&nbsp;Weian Wang,&nbsp;Xiaoqi He","doi":"10.1029/2024JE008720","DOIUrl":"10.1029/2024JE008720","url":null,"abstract":"<p>Wrinkle ridges on Mars, resulting from crustal contraction and tectonic deformation, provide crucial records of tectonic strain. This study presents a possible model based on analog experiments to investigate the influence of varied décollement properties, quantities, and blind thrust faults on the formation of Martian wrinkle ridges. Results indicate that brittle décollements facilitate symmetric ridges with similar primary thrust and backthrust dip angles, whereas ductile décollements promote arch-style ridges with high-angle forelimbs and low-angle backlimbs. Folding is more significant in a single low-viscosity ductile décollement. Blind thrust faults combined with double-layer low-viscosity ductile décollements are crucial for forming typical double ridges, characterized by a broad arch and a narrow ridge. The study suggests that the number, viscosity, distribution of décollements, and rheological properties of décollement influence surface morphology. Comparing these results with Martian observations elucidates factors influencing wrinkle ridge morphology, offering new insights into the tectonic evolution of Martian geological structures and the prediction of potential subsurface décollements, such as those associated with variations in water ice concentrations.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 7","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-07-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144666436","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":"The Diurnal Cycles of Dust and Water Vapor as Observed by EMIRS","authors":"Michael D. Smith,&nbsp;Samuel A. Atwood,&nbsp;Khalid Badri,&nbsp;Christopher S. Edwards","doi":"10.1029/2025JE008972","DOIUrl":"10.1029/2025JE008972","url":null,"abstract":"<p>Thermal infrared spectra taken by the Emirates Mars Infrared Spectrometer (EMIRS) are used to retrieve the diurnal variations of dust optical depth and water vapor column abundance in the Mars atmosphere. Using a retrieval algorithm optimized to determine the effective temperature of these constituents, we can accurately characterize their diurnal variations. Here, we present results from observations taken by EMIRS over more than 1.5 Mars Years. Along with the typical climatological patterns for water ice clouds and water vapor, the EMIRS observations show distinct periods of enhanced dust activity during both Mars Years 36 and 37, with four significant regional-scale dust storms observed but no planet-encircling events. We found small but systematic diurnal variations in both dust and water vapor. Dust optical depth typically increases from mid-morning through early afternoon, reaching peak values in late afternoon before decreasing through the night to minimum values before sunrise. The amplitude of this variation is 0.01–0.02 and is largest at seasons and latitudes where surface temperature is highest. The effective height of the dust layer is about one scale height during the aphelion season but increases to near two scale heights during the perihelion season and higher during dust storms. Water vapor shows modest diurnal variations of ∼10% with column abundance generally increasing during daytime hours, particularly in the morning.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 7","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-07-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144635440","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":"Scour Pits in the Medusae Fossae Formation and Olympus Mons Region on Mars","authors":"Santa L. Pérez-Cortés,&nbsp;Ali M. Bramson,&nbsp;Christina M. Sowinski,&nbsp;Mackenzie Day","doi":"10.1029/2024JE008664","DOIUrl":"10.1029/2024JE008664","url":null,"abstract":"<p>The Medusae Fossae Formation (MFF) covers a region of Mars located to the southwest of the Olympus Mons shield volcano. The nature of this formation has been under debate for over 30 years. In order to better understand the MFF, we investigated scour pits or V-shaped depressions carved into many places across the MFF. We quantified the number and distribution of the scour pits, their length, width, and orientation, and classified them into distinct morphologies: central peak-scour pits, barchan-shaped scour pits, and asymmetric scour pits. We hypothesize that scour pits initially develop as central peak scour pits when wind carves the area around a more resistant obstacle. Therefore, the orientation of the scour pit reflects the orientation of the formative winds. In this study, we found that scour pits in the MFF have similar orientations and morphologies to scour pits found in the north, west, and southwestern flanks of Olympus Mons. These similarities suggest that the scour pits in the MFF and around Olympus Mons are carved into similar materials. We propose that the MFF material extends up to the Olympus Mons region, leading to more MFF material exposed near Olympus Mons than previously mapped. The distribution of scour pits and proximity to Olympus Mons supports previous interpretations that the MFF is pyroclastic in origin.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 7","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008664","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144624812","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":"Influences of Non-Oberbeck–Boussinesq Effects on Tracer Transport in Icy Ocean Worlds","authors":"Shuang Wang,&nbsp;Wanying Kang","doi":"10.1029/2024JE008892","DOIUrl":"10.1029/2024JE008892","url":null,"abstract":"<p>The subsurface oceans on icy satellites are potentially habitable. To understand their habitability, we need to know how tracers with various lifetimes distribute. Convection is the main vehicle for tracer transport, and we expect convection on icy satellites to differ from regular rotating convection, because as pressure increases, water's thermal expansivity can vary by orders of magnitude or even reverse sign near freezing point. Any variation of fluid properties would break the Oberbeck–Boussinesq approximation, leading to non-Oberbeck–Boussinesq (NOB) effects, measured by a coefficient <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>ϵ</mi>\u0000 </mrow>\u0000 <annotation> ${epsilon}$</annotation>\u0000 </semantics></math>. In this work, we identify two competing impacts of NOB effects on tracer transport. The first promotes overall upward tracer transport at <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mi>ϵ</mi>\u0000 <mn>2</mn>\u0000 </msup>\u0000 </mrow>\u0000 <annotation> ${{epsilon}}^{2}$</annotation>\u0000 </semantics></math>-order, while the second enhances transport near the bottom source but inhibits transport further up at <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mi>ϵ</mi>\u0000 <mn>3</mn>\u0000 </msup>\u0000 </mrow>\u0000 <annotation> ${{epsilon}}^{3}$</annotation>\u0000 </semantics></math>-order. In weakly nonlinear regime, the former effect dominates, causing more tracers reaching the ice shell. While in strongly nonlinear regime, the latter effect dominates, reducing tracer concentrations near the ice shell. By varying particle lifetimes, we find that NOB corrections are most pronounced when particle lifetime is comparable to the timescale of upward tracer transport. Additionally, when NOB effects are strong enough to create a stratified layer in the upper part of the ocean, tracer transport into the stratified layer is set by energetics. These effects are expected to prolong the transport timescale of chemical tracers or biosignatures from the seafloor to the ice shell on icy satellites.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 7","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008892","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144624414","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":"Dense Rocks With Smooth Surfaces in Martian Regolith Revealed by Polarimetric Analysis of GPR Data: A Case at Tianwen-1 Landing Site, Mars","authors":"Haoqiu Zhou,&nbsp;Xuan Feng,&nbsp;Zejun Dong,&nbsp;Wenjing Liang,&nbsp;Cai Liu","doi":"10.1029/2024JE008748","DOIUrl":"10.1029/2024JE008748","url":null,"abstract":"<p>This article reports the results of full-polarimetric Mars Rover Penetrating Radar (RoPeR) data acquired by the Zhurong rover of China's Tianwen-1 (TW-1) mission. A modified Freeman decomposition method is applied to the analysis of RoPeR data. By separating different polarimetric scattering components, an imperceptible interface previously obscured by different scattering signals is determined. Besides, an artifact in the signals generated by the double-time reflected signals between the ground and the rover body is identified via correlation analysis. Consequently, a double-layered structure of the Martian regolith to a depth of 3 m is revealed. The shallow layer and deep layer show strong volume scattering power and double-bounce scattering power, respectively, indicating their differences in structure. According to the results of the numerical test, the high-strength signals from the Martian surface are generated by the dense rocks and the undulating terrain, whereas the strong volume scattering components in the regolith are generated by piles of gravel. Besides, a kind of isolated dense rocks with a smooth surface and high loss tangents is identified in the regolith, which is interpreted as the platy duricrusts observed to be formed by aqueous activities. The results demonstrate that the Martian regolith structure at the TW-1 landing site is highly heterogeneous and that aqueous activities may have contributed significantly to it.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 7","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144624416","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":"Global Lunar Boulder Map From LRO NAC Optical Images Using Deep Learning: Implications for Regolith and Protolith","authors":"B. Aussel,&nbsp;O. Rüsch,&nbsp;B. Gundlach,&nbsp;V. T. Bickel,&nbsp;S. Kruk,&nbsp;E. Sefton-Nash","doi":"10.1029/2025JE008981","DOIUrl":"10.1029/2025JE008981","url":null,"abstract":"<p>Boulders on the lunar surface indicate relatively recent surface activity, related to mass wasting or bedrock excavation by impact cratering, and degrade over time, producing regolith. Previously, the distribution of boulders was indirectly assessed using the anisothermality effects observed by the Lunar Reconnaissance Orbiter (LRO) Diviner instrument. Here, we develop a pipeline based on a convolutional neural network to automatically identify and map individual boulders in LRO Narrow Angle Camera (NAC) images between 60°S and 60°N. Using <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 </mrow>\u0000 <annotation> ${sim} $</annotation>\u0000 </semantics></math>635,000 NAC images, we derive the first quasi-global inventory of lunar boulders consisting of about 94 million features with diameters larger than <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mn>4.5</mn>\u0000 </mrow>\u0000 <annotation> $4.5$</annotation>\u0000 </semantics></math> m. We determine relationships between crater diameter and sizes of ejecta boulders and find that the previously known higher boulder density in the mare regions relative to the highlands is due to a preferential location of boulders smaller than <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 </mrow>\u0000 <annotation> ${sim} $</annotation>\u0000 </semantics></math>10 m in the maria. The cumulative boulder size-frequency distributions (CSFDs) of simple crater ejecta are distinct between maria and highlands up to 130 m crater depth. This difference can likely be attributed to distinct subsurface rock contents, with a higher average mature regolith thickness in the highlands compared to the maria. Comparison of the derived boulder data set with the Diviner rock abundance map reveals broad, global agreement yet localized differences, attributable to different sensitivities of the two methods (optical images vs. thermal radiation) and variable geologic context. Diviner-NAC differences pinpoint to distinct lithologies, such as clast-rich zones and zones of fractured impact melt, typically extending for a few hundreds of meters laterally.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 7","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-07-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE008981","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144615361","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}