Journal of Geophysical Research: Planets最新文献

{"title":"Geometry-Dependent Penetration in Microgravity Reveals a Transition From Compaction-Dominated to Shear-Dominated Failure","authors":"G. W. Dai,&nbsp;J. J. Qi,&nbsp;W. W. Mao,&nbsp;Y. Huang,&nbsp;S. H. Xu,&nbsp;H. Yang,&nbsp;Y. S. Hua,&nbsp;L. F. Chen,&nbsp;M. Y. Hou,&nbsp;J. Zhang,&nbsp;H. Zheng","doi":"10.1029/2026JE009850","DOIUrl":"https://doi.org/10.1029/2026JE009850","url":null,"abstract":"<p>Penetration into granular media plays a central role in regolith–structure interactions on planetary bodies, where gravitational acceleration is far lower than on Earth. Although penetration resistance and bearing capacity are commonly inferred from terrestrial experiments, the extent to which reduced gravity alters penetration mechanics and failure behavior remains insufficiently understood. Here, we present a controlled experimental study of quasi-static penetration into dry granular media under terrestrial gravity and microgravity using a drop-tower facility. Penetration resistance, surface deformation, and grain-scale kinematics were measured simultaneously to resolve both macroscopic response and underlying particle motion. The results show that penetration induces compaction of the granular packing under both gravity conditions. However, microgravity leads to markedly different deformation patterns, including enhanced surface rebound, steeper transient slopes, and substantially reduced penetration resistance. Grain-scale displacement fields reveal that these macroscopic differences arise from a gravity-dependent transition in failure behavior: penetration-dominated deformation under terrestrial gravity gives way to shear dilation failure accompanied by vortex-like particle motion under microgravity. These findings demonstrate that penetration behavior observed on Earth cannot be directly extrapolated to low-gravity environments and provide new physical insights into gravity-controlled granular mechanics relevant to planetary surface processes.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 10","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-10-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149206200","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":"Detecting Small-Scale Ionospheric Current Signatures Using MAVEN Observations","authors":"K. G. Hanley,&nbsp;D. A. Brain,&nbsp;T. Weber,&nbsp;D. L. Mitchell,&nbsp;J. Espley,&nbsp;J. S. Halekas,&nbsp;R. Lillis,&nbsp;Ed Thiemann,&nbsp;S. Curry","doi":"10.1029/2026JE009860","DOIUrl":"https://doi.org/10.1029/2026JE009860","url":null,"abstract":"<p>Small-scale (10 s of km) currents in the Martian atmosphere may result in atmospheric heating, ionization, discrete aurora, and atmospheric escape. We have developed a semi-automated method to identify current signatures in the Martian upper atmosphere using perturbations in the local magnetic field. We use magnetic field measurements taken by Mars Atmosphere and Volatile EvolutioN to investigate the incidence of ionospheric current signatures on the nightside of the planet in regions of moderate to strong crustal fields (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>|</mo>\u0000 <mover>\u0000 <mi>B</mi>\u0000 <mo>⃗</mo>\u0000 </mover>\u0000 <mo>|</mo>\u0000 <mo>&gt;</mo>\u0000 </mrow>\u0000 <annotation> $vert vec{mathbf{B}}vert &gt; $</annotation>\u0000 </semantics></math> 25 nT). We find that current signatures are uncommon in horizontal magnetic fields but are detected up to 100% of the time in magnetic cusp regions, where the field is nearly radial. Current signatures are more common post-dusk than predawn, which is consistent with auroral emission. Current signatures are most common in the ionospheric dynamo region, where ion motion is driven by the neutral atmosphere and electrons are bound to magnetic field lines. The occurrence of current signatures does not appear to be influenced by interplanetary magnetic field direction, solar wind dynamic pressure, or solar extreme ultraviolet photon flux.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 10","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149205781","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":"How Large Are Marsquakes? Revisiting Magnitude Scaling and Implications for Marsquakes and Meteoroid Impacts","authors":"Jung-Hun Song,&nbsp;Doyeon Kim,&nbsp;Gareth S. Collins,&nbsp;Victor C. Tsai,&nbsp;Philippe Lognonné","doi":"10.1029/2026JE009988","DOIUrl":"https://doi.org/10.1029/2026JE009988","url":null,"abstract":"<p>Reliable estimates of seismic source size on Mars are critical for interpreting tectonic activity and impact processes, constraining the planet's interior evolution, and informing the design of future Martian seismic experiments. However, because InSight observations are limited to a single station, magnitude estimates cannot rely on empirical averaging of site and path effects as on Earth, and instead depend on comparisons between observed and modeled waveform amplitudes. Consequently, inferred magnitudes are sensitive to assumptions about interior structure, attenuation, and source parametrization. Existing Marsquake Service (MQS) magnitude-scaling relations were calibrated using pre-InSight interior models and tectonic source assumptions, potentially biasing magnitude estimates. Here, we reanalyze spectral amplitudes using InSight seismic data and investigate how post-InSight interior models and source-dependent parametrization influence inferred moment magnitudes. Using waveform simulations for a suite of 1-D interior models, we quantify the effects of velocity structure, attenuation, three-dimensional heterogeneity, and source physics on long-period magnitude scaling. We introduce separate source representations and scaling relations for marsquakes and impacts. Across the tested post-InSight models, the shallow crustal structure beneath InSight primarily controls scaling. Recalibrated marsquake magnitudes are lower by approximately 0.5 <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>M</mi>\u0000 <mi>w</mi>\u0000 </msub>\u0000 </mrow>\u0000 <annotation> ${M}_{w}$</annotation>\u0000 </semantics></math> on average relative to MQS magnitudes, with the reduction varying across plausible shallow structures. Applying impact-specific scaling brings seismic and crater-derived estimates into closer agreement, although differences remain for large distant impacts, and the recalibrated magnitudes enable tentative matching of seismic detections to cataloged Martian impact craters. These relations provide site-specific calibration for InSight observations and tighter constraints on Martian seismicity and impact processes.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 10","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2026JE009988","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149205780","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":"Thermal Conductivity of Iron at the Conditions of Small Planetary Cores","authors":"Eric Edmund,&nbsp;Zachary M. Geballe,&nbsp;Attilio Rivoldini,&nbsp;Nicola Tosi,&nbsp;Stella Chariton,&nbsp;Vitali B. Prakapenka,&nbsp;Alexander F. Goncharov","doi":"10.1029/2025JE009205","DOIUrl":"https://doi.org/10.1029/2025JE009205","url":null,"abstract":"<p>Planetary interiors cool and evolve over geologic time, and their thermal evolution depends on heat transport through their constituent layers. Here, the thermal conductivity of iron has been measured between 19 and 65 GPa and between 1700 and 2500 K in order to constrain its value at the conditions of small planetary cores. Our results are comparable to the low end of electrical resistivity experiments on fcc-Fe at comparable conditions, suggesting that the relationship between electrical and thermal conductivity described by the Wiedemann-Franz law provides a reasonable description of heat transport in fcc-Fe at planetary core conditions. The thermal conductivity of fcc-Fe at high pressures and temperatures places an upper bound on the thermal conductivity of Mercury's core, with a value of 52(7) W/m/K at 40 GPa, which corresponds to the pressure at the center of the core. Accounting for the effects of silicon and sulfur alloying reduces Mercury's core conductivity by 10%–40% for realistic core compositions, which satisfy constraints on Mercury's core density.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 10","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009205","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149205779","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Effects of ICME Composition on the Sputtered Component of the Lunar Exosphere","authors":"A. R. Poppe,&nbsp;Q. Nénon,&nbsp;P. S. Szabo,&nbsp;S. R. Carberry Mogan,&nbsp;C. O. Lee","doi":"10.1029/2026JE009972","DOIUrl":"https://doi.org/10.1029/2026JE009972","url":null,"abstract":"<p>Charged-particle sputtering is a fundamental process that contributes to the generation of the Moon’s neutral exosphere. Neutral sputtering rates are dependent on the speed, flux, and composition of the incident charged-particle populations, all of which are variable at the Moon’s orbit. Dramatic increases in the neutral sputtering rate are likely driven by the impact of interplanetary coronal mass ejections (ICMEs). ICMEs have enhanced densities and speeds, as well as changes in their underlying composition with respect to typical solar wind values. Here, we study the role that ion composition has on the overall contributions to neutral sputtering at the Moon by analyzing in situ observations by NASA’s Advanced Composition Explorer (ACE) mission. A pre-existing catalog of ICMEs at 1 au is used to extract relevant time periods and convolve compositionally resolved ion fluxes with laboratory sputtering yields. Median sputtered fluxes increase by factors of 2.4× and 1.5× the average solar wind value during ICME sheath and ejecta periods, respectively. Protons typically dominate sputtered fluxes from the Moon for all data, including during ICME sheath and ejecta periods; however, the contributions from alphas increases during ICME ejecta due to enhanced alpha-to-proton ratios. Heavy ions, including C, O, Ne, Mg, Si, and Fe typically contribute less than 10% of the total sputtered flux. Furthermore, the relative contribution of heavy ions decreases during ICME ejecta driven by strong increases in the sputtered contribution from alphas. Overall, solar wind heavy ions play an important, although not dominant, role in sputtering of the Moon’s surface.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 10","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-10-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2026JE009972","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149205323","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":"Quantitative Evaluation of Shock Metamorphism in Clinopyroxene Using In Situ X-Ray Diffraction Measurement of Lattice Strain","authors":"Laura E. Jenkins,&nbsp;Roberta L. Flemming,&nbsp;Sam Nicholson,&nbsp;Mark Burchell,&nbsp;Kathryn Harriss,&nbsp;Anne H. Peslier,&nbsp;Roy G. Christoffersen,&nbsp;Jörg Fritz,&nbsp;Cornelia Meyer","doi":"10.1029/2026JE010049","DOIUrl":"https://doi.org/10.1029/2026JE010049","url":null,"abstract":"<p>Shock metamorphism is a ubiquitous process in our solar system. Shock pressure can be related to the lattice strain (<i>ε</i>) of individual minerals within a shocked sample. The lattice strain can be quantified within intact samples by in situ micro-X-ray diffraction (μXRD) using the Williamson-Hall method. The Williamson-Hall lattice strain (W-H <i>ε</i>) method has so far only been calibrated for olivine. This work extends the W-H ε method to high-Ca clinopyroxene. We obtained three sets of experimentally shocked clinopyroxene samples and calculated <i>ε</i> for each sample using μXRD. We created a calibration curve that relates <i>ε</i> to peak shock pressure experienced. Its trend line has the equation <i>P =</i> 222.85<i>ε−</i>8.60 GPa, with an error of ±9 GPa. The calibration curve was applied to the Martian meteorites Nakhla, Zagami, and Allan Hills A77005 (ALHA 77005) to compare these results with the meteorites' optically determined shock stages. The peak shock pressures returned by the calibration curve are: 15 ± 9 GPa for Nakhla, 35 ± 9 GPa for Zagami, and 68 ± 9 GPa for ALHA 77005. These results agree with the meteorites' previously determined shock stages. The development of a W-H ε calibration curve for high-Ca clinopyroxene is preliminary; however, it expands this method for evaluating shock metamorphism of shocked clinopyroxene-bearing samples, such as Martian shergottites.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 10","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2026JE010049","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149146438","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":"Cross-Referencing Astronaut-Observed Lunar Impact Flashes With Seismic Data—Lessons From Apollo for Artemis","authors":"B. Fernando,&nbsp;N. Schmerr,&nbsp;D. Koschny,&nbsp;N. Petro,&nbsp;R. Prabhakhar,&nbsp;A. Deutsch,&nbsp;Y. Nakamura,&nbsp;H. Jack Schmitt","doi":"10.1029/2026JE009762","DOIUrl":"https://doi.org/10.1029/2026JE009762","url":null,"abstract":"<p>During their orbits of the Moon in 1972, Apollo astronauts reported three impact flashes, associated with meteoroids striking the surface and vaporizing. We examined data from the Apollo seismic network to investigate whether these flashes produced detectable moonquakes whose locations and timing could be independently validated. No candidate matches were found, though stream modeling indicates a high probability that both Apollo 17 impacts were Geminids from parent body 3200 Phaethon. Our analysis pipeline is likely instructive for coordinating observations made by future Artemis astronauts from orbit with seismic data from upcoming geophysical missions to the lunar surface.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 10","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2026JE009762","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149146687","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":"Lunar Ring-Moat Dome Structures (RMDSs) in Mare Imbrium: Characterization, Classification, and Implications","authors":"Biao Wang,&nbsp;Feng Zhang,&nbsp;Kaichang Di,&nbsp;James W. Head,&nbsp;Man Peng,&nbsp;Waichuang Liu,&nbsp;Shujuan Sun,&nbsp;Shengli Niu,&nbsp;Ming Jin,&nbsp;Wangbin He,&nbsp;Ziang Su,&nbsp;Bin Xie,&nbsp;Chenxu Zhao,&nbsp;Jing Nan","doi":"10.1029/2026JE009935","DOIUrl":"https://doi.org/10.1029/2026JE009935","url":null,"abstract":"<p>Ring-Moat Dome Structures (RMDSs) are small volcanic landforms in the lunar maria. Although a volcanic origin has been proposed, the controls on their morphological diversity remain unclear. Here, we identify over 3,000 RMDSs in Mare Imbrium (the Moon’s second-largest impact basin) using LROC NAC images, with 2,816 subjected to morphometric analysis based on NAC-derived high-resolution (1 m/pixel) DEMs. These RMDSs have an average diameter of ∼266 m, average height of ∼3.5 m, and a mean height-to-diameter ratio of ∼0.014. Based on dome-moat completeness and relative dome height, we classify them into four classes along with a common subtype. The morphological diversity is mainly attributed to variations in initial magma emplacement processes as well as subsequent volcanic activity and impact gardening. Neither the different classes of RMDSs nor their geometric parameters show obvious spatiotemporal trends, suggesting that differential degradation driven by the interplay of endogenic and exogenic factors may have primarily governed their evolutionary pathways. The density distribution of RMDSs across different mare units and across late-stage lava flows of variable thickness supports the hypothesis that RMDSs originated from magmatic vesiculation and subsequent foam lava extrusion during the late phase of volcanic eruptions. Importantly, we confirm that volatile-rich magma injection during late-stage volcanism, lava flow thickness, and pre-existing topography exert critical controls on RMDS formation and geometry. These findings advance our understanding of lunar volcanism, magma emplacement, and impact modification of volcanic landforms.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 10","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149146439","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":"Décollement Rheology Controls Crustal Deformation on Early Mars","authors":"Oguzcan Karagoz,&nbsp;Jonas B. Ruh,&nbsp;Thomas Kenkmann,&nbsp;Michael H. Poelchau","doi":"10.1029/2026JE010093","DOIUrl":"https://doi.org/10.1029/2026JE010093","url":null,"abstract":"<p>The circum-Tharsis wrinkle ridge system represents one of the strongest tectonic imprints of early Mars, formed as the planet's largest volcanic province reshaped the lithosphere and redistributed stresses across thousands of kilometers. The coherent spatial pattern of these ridges suggests deformation governed by a laterally continuous basal décollement, so that their structural wavelength provides a direct constraint on the rheological state of the early Martian crust. We use thermo-mechanical numerical models to explore two end-member décollement rheologies and their topographic signatures under early Martian conditions. The spacing and characteristic wavelength of circum-Tharsis wrinkle ridges, inferred to have formed during the Early Hesperian, constrain the style and scale of compressional deformation. Frictional décollements, even when weakened by high fluid pressures, are mechanically self-limiting and localize strain, producing only short-wavelength faults that cannot reproduce the observed ridge system. In contrast, low-viscosity décollements (&lt;10¹⁸ Pa·s) distribute stress over long distances and generate regularly spaced, long-wavelength (∼40 km) compressional ridges consistent with the very low surface slopes of Tharsis. These results link volcanic loading and far-field deformation through ductile flow in a weak basal layer, most plausibly rich in salts. The inferred rheology is consistent with extensive evaporite formation on early Mars during Tharsis construction (Noachian to Hesperian), although hydrothermally altered phyllosilicate sequences cannot be excluded on viscosity grounds alone. Our results provide new constraints on crustal composition and hydrothermal conditions during this major phase of Martian tectonic evolution.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 10","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2026JE010093","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149146322","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":"Mesoscale Modeling of Titan’s Shangri-La Region: The Impact of Surface Properties on Winds","authors":"Maxence Lefèvre,&nbsp;Léa E. Bonnefoy,&nbsp;Aymeric Spiga,&nbsp;Bruno de Batz de Trenquelléon,&nbsp;Sébastien Lebonnois,&nbsp;Alexander G. Hayes","doi":"10.1029/2025JE009614","DOIUrl":"https://doi.org/10.1029/2025JE009614","url":null,"abstract":"<p>The knowledge of Titan’s near-surface atmosphere is sparse. The Huygens descent probe measured winds, and the multiple dune field observations and possible dust storms suggest active near-surface dynamics. The Dragonfly rotorcraft lander will fly close to the surface in the Shangri-La region, near the Huygens landing site, where complex dune orientations were observed. This study presents the first mesoscale modeling of the near-surface dynamics in this region. However, due to a lack of high-resolution topography data, synthetic maps of surface properties were built. The surface was divided into different topographical units, such as plains, mountains, etc. The slopes and height of those units were then parametrized. Maps of thermal inertia, albedo and the aerodynamic roughness height were also built. The mesoscale model is coupled to a comprehensive radiative transfer code and forced by a global climate model. No moist processes are considered in this study. Topography has a major impact on near-surface wind amplitude and direction through slope flows and valley circulations. The majority of the winds are below 0.25 m/s. These winds induce a sensible heat flux comparable to the surface solar flux. Spatially varying thermal inertia has the biggest impact on the wind and surface temperature with high values leading to smaller diurnal amplitude. The seasonal variability is taken into account, with stronger winds in northern summer. Predicted mesoscale near-surface winds are capable of lifting dust over dune fields, with different orientations during the year, and can therefore potentially play a role in sediment transport on Titan.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 10","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009614","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149146323","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}