Journal of Geophysical Research: Planets最新文献

{"title":"Ancient Mars Climate With a Polar Ocean and Ice Sheet Dynamics","authors":"Frédéric Schmidt,&nbsp;Michael J. Way,&nbsp;Aurélien Quiquet,&nbsp;Igor Aleinov,&nbsp;Christophe Dumas","doi":"10.1029/2025JE008970","DOIUrl":"https://doi.org/10.1029/2025JE008970","url":null,"abstract":"<p>In this article, we study the conditions required to maintain a stable ocean on Mars 3 Ga using a new suite of simulations. These simulations couple a 3D Global Climate Model with ocean dynamics and ice sheet flow. The model includes the main processes of the atmosphere/hydrosphere/cryosphere to investigate Mars' ancient climate. The results show that the total water content required to maintain an ocean is <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 <mn>700</mn>\u0000 </mrow>\u0000 <annotation> ${sim} 700$</annotation>\u0000 </semantics></math> m, global equivalent layer, half in the ocean, half in the ice sheet. This number seems plausible if a significant amount of water has been absorbed by the ground. This could be in the form of mineral alteration, or in a deep porous reservoir. In addition, the results show that the equilibrium mass flux from the ice sheet adjacent to the northern ocean is <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 <mn>1</mn>\u0000 <msup>\u0000 <mn>0</mn>\u0000 <mn>15</mn>\u0000 </msup>\u0000 </mrow>\u0000 <annotation> ${sim} 1{0}^{15}$</annotation>\u0000 </semantics></math> kg/y with a very low sliding velocity (1 m/y), except for few warm regions in the lowest altitudes that could reach up to 300 m/y. Finally, the global atmosphere/hydrosphere/cryosphere equilibrium should be reached in a few 100 ky. This indicates that the ocean will have a stabilizing feedback on timescales longer than this. An extensive sensitivity study of the ice sheet was performed. This included the effects of a geothermal heat flux, viscosity and basal drag. Finally, we studied the possible effects of planetary obliquity and a reduced ocean extent.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 10","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-10-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE008970","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145223894","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":"Electrical Resistivity of Liquid Fe-16S-2Si up to 13 GPa With Implications for the Adiabatic Heat Flux Through the Core of Exoplanet TRAPPIST-1h","authors":"E. M. Lenhart,&nbsp;W. Yong,&nbsp;R. A. Secco","doi":"10.1029/2025JE009203","DOIUrl":"https://doi.org/10.1029/2025JE009203","url":null,"abstract":"<p>Thermal convective processes in the liquid cores of terrestrial planetary bodies with the capacity to generate magnetic dynamos may be better characterized by thermal conductivity estimates of core conditions. The composition of the core of asteroid 4 Vesta as determined by geochemical studies of HED meteorites is used as an analog for the core of exoplanet TRAPPIST-1h. Earlier electrical resistivity measurements of the Fe-S-Si system up to 6 GPa are extended here to 13 GPa using a 3,000-ton multi-anvil press. Data were collected from ambient temperatures to ∼2,000 K in each experimental run. Temperature and voltage drop across the sample were measured in situ to derive resistivity from geometry measurements of the post-experimental sample cross-section. At temperatures above the liquidus of Fe-16 wt%S–2 wt%Si, the electrical resistivity is 400–500 μΩ cm and is invariant in the pressure range 5–13 GPa. From the Wiedemann-Franz Law, the electronic contribution to the thermal conductivity is calculated as 8–10 W/m/K at the completion of melting. The adiabatic heat flux at the top of the core of TRAPPIST-1h is estimated as 5.3 ± 2 or 6.8 ± 3 mW/m² in the case of a surface ice layer. For a critical value of the magnetic Reynolds number of 10, a characteristic velocity in the core of ∼0.02 mm/s is required. With selected parameter values for the core of TRAPPIST-1h, this velocity value is likely achieved by convective heat flux, sustaining a magnetic dynamo.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 10","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-10-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009203","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145223777","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":"Using Venus, Earth, and Mars to Understand Exoplanet Volatile and Climate Evolution","authors":"Bruce M. Jakosky,&nbsp;Paul K. Byrne","doi":"10.1029/2024JE008882","DOIUrl":"https://doi.org/10.1029/2024JE008882","url":null,"abstract":"<p>Venus, Earth, and Mars exhibit a wide range of interactions between their deep interiors, surfaces, lower and upper atmospheres, and the Sun, with commensurate variations in the nature of their atmospheres and evolution of their volatiles. By examining these worlds' characteristics and behavior, we can gain some understanding of the breadth of possibilities for the evolution of volatiles on rocky exoplanets. Doing so is especially important because we cannot predict in advance of direct observations how a terrestrial planet will respond to its solar- or stellar-system boundary conditions and to its interior properties and what the outcome will be. Exoplanet volatile evolution depends strongly on the geological and geophysical behavior of the planet in addition to the ability of the host star to strip away atmosphere, and the interplay between stellar and geological influences depends greatly on the timescales on which each process varies. A planet's numerous ways to sequester gas out of the atmosphere and to recycle it back into the atmosphere suggests that estimates of planetary surface conditions and even habitability based only on the stellar stripping of gas are likely to be vastly oversimplified and probably incorrect.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 10","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008882","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145223953","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":"Global Energy Transport and Conversion in the Solar Wind-Mars Interaction: MAVEN Observations","authors":"Chi Zhang,&nbsp;Chuanfei Dong,&nbsp;Hongyang Zhou,&nbsp;Jasper Halekas,&nbsp;Xinmin Li,&nbsp;Jiawei Gao,&nbsp;Han-Wen Shen,&nbsp;Xiao-Dong Wang,&nbsp;Hans Nilsson,&nbsp;Robin Ramstad,&nbsp;Christian Mazelle,&nbsp;Liang Wang,&nbsp;Shaosui Xu,&nbsp;Abigail Tadlock,&nbsp;Kathleen G. Hanley,&nbsp;Shannon M. Curry,&nbsp;David L. Mitchell","doi":"10.1029/2025JE009295","DOIUrl":"https://doi.org/10.1029/2025JE009295","url":null,"abstract":"<p>The interaction between the solar wind and Mars plays a crucial role in driving atmospheric escape and shaping the Martian space environment. Despite its importance, the electromagnetic energy transport and conversion associated with this interaction remain poorly characterized. In this study, we construct global maps of electromagnetic energy transport and conversion at Mars using 9 years of magnetic field and plasma data from NASA's Mars Atmosphere and Volatile EvolutioN (MAVEN) mission. Our results reveal that the bow shock serves as an electromagnetic generator, converting the kinetic energy of the solar wind into electromagnetic energy. In contrast, the induced magnetotail acts as a load region, where electromagnetic energy is converted back into particle energy. The magnetosheath exhibits a spatially variable role: it functions as a generator in regions where the interplanetary magnetic field (IMF) is draped around the planet but transitions into a load region as the draped fields are diverted toward the magnetic poles. Planetary oxygen ions are persistently energized throughout the system, with particularly strong energization observed in the ion plume region. We also identify a pronounced hemispheric asymmetry in energy transport and conversion. While our qualitative results are robust, the quantitative analysis reveals an imbalance between the calculated energy transport and conversion terms. This discrepancy suggests that unresolved small-scale electric fields or currents and nonlinear processes may be missing from the present analysis, underscoring the need for future high-resolution, multi-point observations to better constrain the electromagnetic energy budget and enhance our understanding of the Martian space environment.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 10","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145224047","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":"Particle in Cell Simulation on Mode Conversion of Saturn's 20 kHz Narrowband Radio Emission","authors":"Zhoufan Mu,&nbsp;Yao Chen,&nbsp;Tangmu Li,&nbsp;Sulan Ni,&nbsp;Zilong Zhang,&nbsp;Hao Ning","doi":"10.1029/2024JE008899","DOIUrl":"https://doi.org/10.1029/2024JE008899","url":null,"abstract":"<p>The Z-to-O mode conversion at the density gradient is the prevailing mechanism of narrowband (NB) radio emission in planetary magnetosphere. Most previous numerical models were for NB emission observed in the Earth magnetosphere, using the cold plasma fluid approximation that excluded any kinetic effect. Here we investigate the Z-to-O conversion process underlying the Saturn's 20 kHz NB emission, using the fully kinetic and electromagnetic particle-in-cell (PIC) simulation. We simulate the whole process starting from the pumping of the Z mode, to its propagation and reflection, and further conversion into the O mode radiation. The energy conversion rate of the Z-to-O process is estimated to be 10%–20%. This provides the first quantitative estimate of such rate with PIC simulations.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 10","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145224048","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":"Mineralogically Diverse and Salt-Rich Regolith in Jezero Crater Characterized Using X-Ray Spectroscopy","authors":"Andrew O. Shumway,&nbsp;Tanya V. Kizovski,&nbsp;David C. Catling,&nbsp;Scott J. VanBommel,&nbsp;Michael W. M. Jones,&nbsp;Brendan J. Orenstein,&nbsp;Mariek E. Schmidt,&nbsp;Michael M. Tice,&nbsp;Joel A. Hurowitz,&nbsp;Abigail L. Knight,&nbsp;Benton C. Clark,&nbsp;Lawrence Wade,&nbsp;Emily L. Cardarelli,&nbsp;An Y. Li,&nbsp;Mike J. Zawaski,&nbsp;David A. Klevang,&nbsp;William T. Elam,&nbsp;Elisabeth M. Hausrath,&nbsp;Allan H. Treiman,&nbsp;Jesper Henneke,&nbsp;Nicholas J. Tosca,&nbsp;Yang Liu,&nbsp;Morgan L. Cable,&nbsp;Abigail C. Allwood","doi":"10.1029/2024JE008912","DOIUrl":"https://doi.org/10.1029/2024JE008912","url":null,"abstract":"<p>The Planetary Instrument for X-ray Lithochemistry (PIXL) onboard the Perseverance rover has characterized the composition of Martian regolith at a scale of hundreds of microns using micro-focus X-ray fluorescence spectroscopy. PIXL data reveal a diverse population of regolith grains with distinct spectral, chemical, and crystallographic properties, through which we identified the mineralogy of individual regolith components. Olivine, phyllosilicate, carbonate-bearing phases, Cr-Ti-spinel, plagioclase, and Fe-sulfate are all inferred from the data, and potential local and regional bedrock sources are proposed for each. PIXL also inspected dust and soil components, which were found to be geochemically similar to analogous components characterized elsewhere by preceding missions. Unlike other sites, regolith on the western fan front of Jezero crater contains fewer sulfates, but is highly enriched in Cl (up to 2.0 ± 0.5 wt. %), which likely includes chlorides, chlorates, and/or perchlorates. PIXL also finds evidence of hydration in the regolith, potentially carried by salts, as interstitial water, and/or in adsorbed phases. PIXL's observations of diverse amorphous and crystalline components, multiple styles of aqueous alteration, and enrichments of brine-forming salts provide exciting new justification for the return of a Martian regolith sample to Earth for further study.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 10","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008912","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145224500","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":"Potential Source Depth of Pure Plagioclase Exposed at Peak Rings of Impact Basins on the Moon","authors":"Guo-Hua Xu,&nbsp;Meng-Hua Zhu,&nbsp;Xi-Zi Luo,&nbsp;Min Ding,&nbsp;Luyuan Xu,&nbsp;Kai Wünnemann","doi":"10.1029/2025JE009323","DOIUrl":"https://doi.org/10.1029/2025JE009323","url":null,"abstract":"<p>The lunar magma ocean (LMO) hypothesis suggests that the Moon's primary crust is largely composed of pure plagioclase; however, only limited pure plagioclase outcrops on the lunar surface were detected from the remote sensing observations. The spectral observations show that most crystalline plagioclase-rich features are concentrated on the peak rings of large basins, indicating that they were likely originally buried beneath the surface and then excavated by the formation of those basins. However, the potential source depths of these exposed pure plagioclase outcrops remain unconstrained. In this work, we aim to estimate the pre-impact depth of the observed pure plagioclase via numerical simulation of peak ring basin formation, which allows tracing the pre-impact depth of peak rings in basins of various sizes. According to our systematic modeling, we propose a power-law scaling function that links the potential source depth of pure plagioclase at peak rings to the basin diameter. Our results suggest that the observed pure plagioclase on the peak-ring basins in the Feldspathic Highlands Terrane originates from depths of ∼20–30 km below the surface. This layer of pure plagioclase is thought to be part of the primary crust that was formed during LMO crystallization. Our results advance the understanding of the structure and evolution of the lunar crust, and provide a framework that can be used to investigate the crustal structure of other solid planetary bodies.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 10","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145146610","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":"Re-Analysis of Pioneer Venus Data: Water, Iron Sulfate, and Sulfuric Acid are Major Components in Venus' Aerosols","authors":"R. Mogul,&nbsp;M. Yu. Zolotov,&nbsp;M. J. Way,&nbsp;S. S. Limaye","doi":"10.1029/2024JE008582","DOIUrl":"https://doi.org/10.1029/2024JE008582","url":null,"abstract":"<p>We present a new and transformative composition for Venus' cloud aerosols using previously uncharacterized data acquired by the Pioneer Venus Large Probe, which descended through Venus' atmosphere in 1978. This aerosol composition was extracted by re-analyzing data acquired by the Large Probe Neutral Mass Spectrometer (LNMS) and re-evaluating results from the Large Probe Gas Chromatograph (LGC). In our approach, the altitude-based data from the LNMS and LGC were re-interpreted as the thermal and evolved gas analysis of aerosol composition. During the descent, the LNMS and LGC inadvertently collected cloud aerosols and subsequently measured the release of gases and compounds as the captured aerosols thermally decomposed across the hot sub-cloud atmosphere. Evolved compounds that were released into the LNMS included SO₂, H₂O, SO₃, O₂, and likely Fe₂O₃ and MgSO₄. Evolved gases that were released into the LGC included SO₂, H₂O, and O₂, which likely formed during the programmed LGC heating steps. These results are consistent with the thermal decomposition of aerosols containing comparable masses of ferric sulfate and sulfuric acid (∼20 wt%, each) and sufficiently high H₂O abundances (∼60 wt%) to yield hydrated iron sulfates, hydrated magnesium sulfate, and other hydrates. We suggest that iron and magnesium could originate from cosmic sources. Our comparisons indicate that aerosol H₂O was also measured by direct analyses on the Venera and Vega probes. Hence, this work reveals reservoirs of water and possible altered cosmic materials in the aerosols, which presents new considerations for cloud chemistry and cloud habitability models.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008582","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145146416","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":"Influence of Lateral Shear on the Formation of Enceladus' South Polar Terrain","authors":"Y. Jin,&nbsp;S. Chen,&nbsp;A. Yin,&nbsp;H. Zhang,&nbsp;Y. Shi","doi":"10.1029/2024JE008860","DOIUrl":"https://doi.org/10.1029/2024JE008860","url":null,"abstract":"<p>Structural mapping indicates that Enceladus' South Polar Terrain (SPT) has experienced a regional-scale right-lateral shear, but the precise role of the regional shear in SPT's evolution is still under debate. Here we investigate the effects of lateral shear with a three-dimensional visco-elasto-plastic model. By presetting a circular thinned lid around the south pole, we have obtained numerical results in good agreement with the general tectonic pattern of today's SPT, which explain the formation mechanism for some of the peculiar structures in the SPT. Our results suggest an inward cascading procedure in initiating the Tiger Stripes, wherein the fracturing starts at the rim of the thinned lid. Furthermore, we put forward the potential existence of ancient Riedel shear zones that pass through the tips of the Tiger Stripes, which may correspond to the strips with low albedo in infrared band in the albedo maps of the SPT.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 10","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145146707","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 Boulder-Rich Blocky Unit of the Western Jezero Upper Fan: Discriminating Olivine and Pyroxene Compositions and Constraining Provenance","authors":"Alicia F. Vaughan,&nbsp;Melissa Rice,&nbsp;Athanasios Klidaras,&nbsp;Jeffrey R. Johnson,&nbsp;Samantha Gwizd,&nbsp;Briony Horgan,&nbsp;Linda C. Kah,&nbsp;Opal Cianciolo,&nbsp;Gerhard Paar,&nbsp;James Bell III","doi":"10.1029/2025JE009159","DOIUrl":"https://doi.org/10.1029/2025JE009159","url":null,"abstract":"<p>The boulder-rich unit of the Upper Western Fan in Jezero crater, Mars is the youngest preserved unit of the fan stratigraphy. Understanding boulder compositions, distribution, and textures is critical for constraining their emplacement, provenance, and the depositional history of the Western fan. We use Mastcam-Z multispectral images to identify and discriminate between two compositions of boulders: olivine- and pyroxene-bearing. Spectral parameters distinguish endmembers from other geologic units investigated by the Perseverance rover within Jezero crater and indicate a distinct provenance. We map the distribution of each type across distinct lobes of the fan, characterize their morphology, and use WATSON images to interpret grain-scale textures. Differences in type-distribution among lobes of the fan supports the distinction of those lobes as previously mapped. The olivine-bearing boulders are dominant across the unit with rounded shapes consistent with fluvial deposition sourced from the regional olivine unit. Less populous and rougher pyroxene-bearing boulders may have been emplaced through a shorter fluvial transport distance from the pyroxene-bearing crater rim deposits, or as possible impact ejecta. This work supports earlier claims that high-energy fluvial activity played a role in the later stages of the Western Fan formation in Jezero crater. Ongoing and future exploration of the Jezero crater rim will allow further study and evaluation of potential source regions for the boulders of the Western Jezero fan top.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 10","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009159","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145146587","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}