Journal of Geophysical Research: Planets最新文献

{"title":"Microstructural Analysis of Lunar Dunite Clast From Meteorite NWA 11421 and Physical Constraints on Excavation of Upper Lunar Mantle Material","authors":"I. Spring,&nbsp;T. Erickson,&nbsp;A. Mallik,&nbsp;A. Roy,&nbsp;A. Treiman","doi":"10.1029/2026JE009689","DOIUrl":"https://doi.org/10.1029/2026JE009689","url":null,"abstract":"<p>Lunar dunite clast, D1, from lunar meteorite NWA 11421 represents the first lunar sample that potentially traces back to the lunar mantle and may provide insights into the Moon's interior structure and chemistry. We conducted electron backscatter diffraction (EBSD) analysis of the clast to characterize its olivine microstructures and preferred orientations and to quantify its shock history. The EBSD data indicate that D1 olivine grains are generally elongate with a moderate shape preferred orientation and a weak B-type crystallographic preferred orientation. Intragrain misorientations indicate that D1 experienced a high-pressure, low-temperature shock event. Grain orientation spread (GOS) indicates a weighted shock stage of 4.1 ± 1.3, corresponding to shock pressures of 15–20 GPa. Crystallographic rotation axes associated with low-angle (2–10°) misorientations demonstrate preferential activation of C-type slip, consistent with the relatively low shock temperatures of 720 ± 99°C that were estimated using previously published linear relationships of experimentally shocked olivine. Notably, this shock temperature is below the sample's equilibrium temperature of 980 ± 20°C, as determined by two-pyroxene thermometry. This contrast suggests that the thermal state achieved during shock was conducive to preserving the primary mantle chemistry. The olivine fabric within D1 displays J- and M-indices consistent with other shocked meteorites; notably, the M-index of these meteorites is lower than that of terrestrial mantle xenoliths. Combined with the sample's depth of origin, these characteristics suggest D1 was excavated from either the Imbrium or Serenitatis basins and may provide the first chemical constraints on nearside lunar mantle.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 8","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-08-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148784260","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 Impact of Data Resolution on Planetary Compressional Structure Analysis","authors":"F. Carboni","doi":"10.1029/2026JE009794","DOIUrl":"https://doi.org/10.1029/2026JE009794","url":null,"abstract":"<p>Planetary studies of compressional structures are fundamental for understanding the tectonics and thermal evolution of planetary bodies. Compressional features are commonly characterized by their morphology, which in turn is strongly dependent on the spatial resolution of topographic data. Low-resolution data may lose important morphological characteristics that are directly linked to their structural architecture. Although the influence of data resolution in the analysis of surface structures is widely recognized, a systematic and comparative quantification of shortening over- or underestimation across different morphologies and resolutions is still lacking, and the amount of these deviations remains quantitatively poorly constrained. In this work, I assess the effect of data resolution on the morphological and structural analysis of five compressional ridges with different sizes and geometries on Mars using four digital elevation models with different resolutions: Mars Orbiter Laser Altimeter (∼463 m/px), High-Resolution Stereo Camera (∼75–∼100 m/px), CTX (∼6 m/px), and HiRISE (∼0.3 m/px). Additional applications to one example on Venus and one on Mercury are used to evaluate transferability to other planetary bodies. The results quantitatively demonstrate how morphological characterization and structural analysis can be affected by significant local deviations depending on the size of the analyzed structures and the type of topographic data. By applying a harmonic index to ridge width and relief on Mars, I identify a threshold range of approximately ∼175–275 m. Below it, low-resolution data become unreliable, whereas above it, they can provide an overall reliable characterization. Based on the current available data sets, this threshold appears valid on Mars and potentially on Venus, but apparently not on Mercury.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 8","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-08-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2026JE009794","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148753617","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":"Characteristics of Lunar Surface Electrons Inferred From THEMIS-ARTEMIS Observations: 2. Photoelectrons","authors":"Shaosui Xu,&nbsp;Andrew R. Poppe,&nbsp;Yuki Harada,&nbsp;Phillip C. Chamberlin","doi":"10.1029/2026JE009879","DOIUrl":"https://doi.org/10.1029/2026JE009879","url":null,"abstract":"<p>The lunar surface charging is controlled mainly by the balance of electron currents near the surface. One of the main electron currents is the photocurrent on the dayside, comprised of photoelectrons produced by solar photons ionizing the lunar surface. Yet, there lacks a systematic characterization of the statistical properties of lunar photoelectrons. Photoelectrons can be uniquely identified by the oxygen Auger electron flux peak in the photoelectron energy spectrum. In this study, we develop a methodology to select lunar photoelectron measurements from the Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) mission. With such a photoelectron database, we statistically analyze several properties of the lunar photoelectrons when the Moon is in the magnetotail lobe environment and in the solar wind environment, including how the photoelectron fluxes and the photoelectron detection probability vary and depend on driving parameters.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 8","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-08-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2026JE009879","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148943209","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":"Mars' Dayside Induced Magnetosphere Under Quasi-Radial Interplanetary Magnetic Field—A MHD Model Study","authors":"Yihui Song,&nbsp;Haoyu Lu,&nbsp;Jinbin Cao,&nbsp;Shibang Li,&nbsp;Xiaoshu Wu,&nbsp;Jianxuan Wang,&nbsp;Nihan Chen,&nbsp;Yasong Ge,&nbsp;Yuchen Cao,&nbsp;Jianing Zhao","doi":"10.1029/2026JE009816","DOIUrl":"https://doi.org/10.1029/2026JE009816","url":null,"abstract":"<p>The interplanetary magnetic field (IMF) is one of the important external drivers that control the Martian plasma environment. There is some controversy about the characteristics of the Martian plasma environment under radial IMF conditions. Utilizing a three-dimensional magnetohydrodynamic (MHD) model, this study analyzes the impact of IMF cone angle on the electromagnetic field and ion motions in Martian space, and investigates the Martian space environment under radial IMF conditions. Simulation results indicate that the decrease in IMF cone angle weakens the electromagnetic fields. The reduction in magnetic field pile-up leads to a weakened induced magnetosphere. Therefore, solar wind protons experience less deceleration and deflection across the bow shock (BS), which is compressed to lower altitudes. Under radial IMF, though the electric fields that impede the penetration of solar wind particles are weak on the dayside, the BS, the magnetosheath, and the induced magnetosphere structure can still form, and the pile-up of magnetic fields can still be observed. In contrast to previous reports of BS disappearance under radial IMF, our simulations show that a BS and a structured magnetosheath persist even at extremely small cone angles. These results help reconcile conflicting observations and provide constraints for interpreting MAVEN measurements during near-radial IMF intervals.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 8","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-08-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148753789","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 Length of Martian Crater Rays and Their Relation to Lunar Cold Spots","authors":"Trevor P. Erwin,&nbsp;Brandon C. Johnson,&nbsp;David Minton,&nbsp;Alexandria V. Johnson","doi":"10.1029/2025JE009609","DOIUrl":"https://doi.org/10.1029/2025JE009609","url":null,"abstract":"<p>Impact-generated crater rays are well-documented on the Moon, with most appearing as high-albedo streaks extending radially from a crater's center. On Mars, however, crater rays are significantly rarer and discernible only through thermal imaging due to their lower thermal inertia compared to surrounding terrain. This study presents the first comparative analysis between the lengths of Martian and lunar crater rays, including lunar albedo rays and cold spots, which are ray-like thermal anomalies associated with many of the youngest lunar craters. Our findings indicate that both Martian crater rays and lunar cold spots extend significantly farther than lunar albedo rays, with lengths an order of magnitude greater for craters of equivalent diameter. Furthermore, we propose a connection between the formation mechanisms of Martian crater rays and lunar cold spots based on their thermal properties. By integrating thermal rays into existing ejecta models, we refine the understanding of crater-ray formation and suggest that Martian crater rays and lunar cold spots may share a similar formation mechanism via secondary cratering processes. Advancing knowledge of these features has implications for impact dynamics and surface evolution across planetary bodies.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 8","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-08-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009609","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148753729","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":"Subsurface Structure and Morphometry of the Wrinkle Ridges in the Late Amazonian Volcanic Unit on Mars","authors":"Jianfei Liu,&nbsp;Lu Pan","doi":"10.1029/2025JE009623","DOIUrl":"https://doi.org/10.1029/2025JE009623","url":null,"abstract":"<p>Wrinkle ridges are widespread compressional tectonic features on Mars and are important records of the planet's global contractional history. However, their formation, evolution and subsequent modification by other geologic processes remain poorly constrained. Combining radar data, elevation data and high-resolution imagery, we find that the uppermost layer of the Late Amazonian volcanic (lAv) unit is ∼50 m thick and exhibits dielectric properties consistent with porous basalt (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mi>ε</mi>\u0000 <mo>′</mo>\u0000 </msup>\u0000 </mrow>\u0000 <annotation> ${varepsilon }^{prime }$</annotation>\u0000 </semantics></math> = 7.50 ± 0.69; <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>tan</mi>\u0000 <mspace></mspace>\u0000 <mi>δ</mi>\u0000 </mrow>\u0000 <annotation> $tan ,delta $</annotation>\u0000 </semantics></math> = 0.011–0.077). Stratigraphic analyses and crater dating within the Amazonis Planitia west of Olympus Mons reveal multiple resurfacing events at ∼1.3 Ga, ∼240 Ma, and ∼28 Ma. The estimated volume of the youngest flow is ∼7.50 × 10⁴ km³, and flow thicknesses appear to have progressively decreased over time. Radar and image data demonstrate that the latest lava flow completely buried the preexisting ridges while preserving their subsurface geometry. Wrinkle ridges within the lAv unit differ from global averages, showing enhanced widths, lower heights, larger width-to-height ratios, and reduced elevation offsets. These morphometric deviations suggest substantial post-formational modification by volcanic flooding, topography inflation and sedimentation with potential contributions from varying fault geometry and slip. The modification may have led to an underestimation of derived strain by up to ∼22%. These findings reveal that volcanism both alters surface ridge topography and preserves underlying structure, emphasizing the necessity of radar constraints to reconstruct tectonic history on Mars.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 8","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-08-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009623","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148753347","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":"Surface Thermal Tides and Radiative Adjustment in Venus's Deep Atmosphere","authors":"Rachel Navon,&nbsp;Eli Galanti,&nbsp;Sebastien Lebonnois,&nbsp;Ehouarn Millour,&nbsp;Yohai Kaspi","doi":"10.1029/2026JE009679","DOIUrl":"https://doi.org/10.1029/2026JE009679","url":null,"abstract":"<p>Thermal tides on Venus have been extensively studied near the cloud tops, where their three-dimensional structure and contribution to the atmospheric momentum budget have been characterized from temperature and wind fields. However, their downward propagation and influence within the deep atmosphere remain uncertain, and their behavior in the deep atmosphere, particularly near the surface, remains poorly constrained. Using the LMD Venus Planetary Climate Model, we investigate the near-surface thermal tides and their governing timescales. The simulations show that these tides are generated by heat transfer from the surface to the planetary boundary layer and produce a diurnal pressure response with a phase lag of about <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mn>30</mn>\u0000 <mo>°</mo>\u0000 </mrow>\u0000 <annotation> $30{}^{circ}$</annotation>\u0000 </semantics></math> corresponding to a radiative adjustment timescale of about 10 Earth days. In addition, a 35-day oscillation appears within the stably stratified 10–20 km layer, consistent with a planetary-scale internal gravity wave. These results suggest that coherent oscillations beyond the diurnal tide can develop in the deep atmosphere, with the surface pressure variability dominated by a superposition of three modes: the diurnal and semidiurnal tides and the 35-day oscillation. Together, these components account for about 70<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>%</mi>\u0000 </mrow>\u0000 <annotation> $%$</annotation>\u0000 </semantics></math> of the total surface pressure variance, with potential implications for gravity measurements by forthcoming missions such as VERITAS and EnVision.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 8","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-08-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2026JE009679","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148753296","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":"What Earth Erases: Weathering Diversity of Mineral Phases Formed in a Highly Reduced Environment Hosted in Aubrites","authors":"M. Kołodziej,&nbsp;B. Pieterek,&nbsp;G. Zieliński,&nbsp;K. Załęski,&nbsp;E. Coy","doi":"10.1029/2026JE009937","DOIUrl":"https://doi.org/10.1029/2026JE009937","url":null,"abstract":"<p>Meteorites serve as an exceptional source of insight into our planet and the Solar System. Most meteorite fragments were recovered hundreds to thousands of years after their fall, and therefore exhibit varying degrees of terrestrial weathering, which has altered or completely removed weather-sensitive mineral phases. This study focuses on two aubrites—NWA 14582 and Ribbeck—examining the differences in their mineral composition. The NWA 14582 was collected in a desert long after its fall and has undergone significantly greater shock metamorphic alteration than the Ribbeck meteorite. The alterations are evidenced by the structural changes in its enstatite and diopside, along with the absence of feldspars, which have transformed into maskelynite. The Ribbeck meteorite, recovered shortly after its descent, revealed several mineral phases not present in NWA 14582. Electron microprobe investigations confirmed that minerals such as troilite, daubréelite, schreibersite, and kamacite exhibit resistance to weathering. Conversely, the observed minerals, such as heideite, caswellsilverite, oldhamite, pentlandite, and alabandite, appear to be particularly susceptible to terrestrial weathering processes. Our observations further indicate that the climate at the fall site can have a substantial impact on the preservation of primary mineral phases and the formation of secondary weathering products. We additionally report a Cu-based iodide in an early sample preparation that was not preserved in subsequently prepared mounts, as well as a rare Al–Cu–Zn alloy in Ribbeck. Further microchemical and isotopic analyses are required to determine the provenance of these phases.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 8","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-08-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2026JE009937","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148753405","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":"Developing and Characterizing a New-generation Regolith Simulant “IGCAS-AST01” for the Tianwen-2 Target Asteroid (469219) Kamoʻoalewa","authors":"Pengfei Zhang,&nbsp;Zichen Wei,&nbsp;Takahiro Hiroi,&nbsp;Jin Zhao,&nbsp;Edward Cloutis,&nbsp;Guozheng Zhang,&nbsp;Marco Fenucci,&nbsp;Rui Li,&nbsp;Xiaojing Zhang,&nbsp;Xiaoping Zhang,&nbsp;Zhiping He,&nbsp;Yan Su,&nbsp;Yangting Lin,&nbsp;He Zhang,&nbsp;Yang Li","doi":"10.1029/2026JE009859","DOIUrl":"https://doi.org/10.1029/2026JE009859","url":null,"abstract":"<p>China plans to return samples from the near-Earth asteroid (469219) Kamoʻoalewa, which we previously identified as an LL-chondrite-compositional, highly space-weathered object with fine-grained regolith. In this study, we developed 10 mL of Kamoʻoalewa regolith simulant, designated “IGCAS-AST01,” by irradiating LL5/6 chondrite (Kheneg Ljouâd) powder with a high-energy pulsed laser. We then analyzed the composition, grain size distribution, density, porosity, visible to near-infrared reflectance spectrum, emission spectrum (approximated as 1–Reflectance), thermal diffusivity, specific heat capacity, and microstructural features of both the fresh (unirradiated) powder and IGCAS-AST01. IGCAS-AST01 is composed of 57.8 vol.% olivine, 19.9 vol.% orthopyroxene, 5.6 vol.% diopside, 12.2 vol.% plagioclase, 2.6 vol.% troilite, and minor amounts of other phases. It has a mean size of 26.99 μm, a median size of 23.19 μm, a density of 1196.8 kg m⁻³, and a porosity of 64.3%. Additionally, IGCAS-AST01 exhibits a low reflectance of 0.1 at 0.55 μm and an extremely steep spectral slope. In the temperature range of 253.15–473.15 K, its thermal diffusivity and specific heat capacity range from 3.6–4.7 × 10⁻⁶  m² s⁻¹ and 718.43–890.20 J kg⁻¹ K⁻¹, respectively. Furthermore, thick amorphous rims and abundant nanophase metallic iron particles are observed in olivine and pyroxene grains of IGCAS-AST01. These results could support the Tianwen-2 mission's payload calibration, sampling operations, on-orbit scientific data interpretation, and future sample analysis.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 8","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-08-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148753406","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":"Surface Stability Predictions of Sublimating Ice-Covered Worlds via the Optimization of Surrogate Neural Networks: Application to Europa","authors":"A. Macias,&nbsp;A. Hsu,&nbsp;D. Mavris,&nbsp;D. Berisford,&nbsp;M. S. Bramble,&nbsp;D. Goldstein,&nbsp;P. Varghese,&nbsp;L. Trafton,&nbsp;K. P. Hand","doi":"10.1029/2025JE009389","DOIUrl":"https://doi.org/10.1029/2025JE009389","url":null,"abstract":"<p>The morphology of the surface ice on Europa remains unknown at the meter scale. Hobley et al. (2018, https://doi.org/10.1038/s41561-018-0235-0) suggested the possible presence of penitentes—bladed ice structures that form on Earth—on the surface of Europa, based on analogy to Earth. Characterized as instability features, penitentes grow due to differential sublimation erosion and ablation of a snowfield. Previous studies have provided contrasting results when examining the stability of the terrain on Europa from isolated radiative heat transfer and molecular transport mechanisms. We analyze these mechanisms simultaneously, leveraging Physics-Informed Neural Networks to identify physical conditions and suitable terrains that could potentially host centimeter-to meter-scale ridges and penitentes on Europa. We find that for the specific condition of a pre-defined sinusoidal ice morphology, values of ice thermal inertia near the lower limit of physically plausible values for low density, pure water ice may lead to the growth of features such as penitentes. Conversely, higher values of thermal inertia may lead to erosion of morphologies and convergence toward a flat surface. Our results can help inform the interpretation of NASA Europa Clipper and ESA Jupiter Icy Moons Explorer (JUICE) observations, and help guide landing site selection for future missions to the surface of Europa.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"131 8","pages":""},"PeriodicalIF":3.7,"publicationDate":"2026-08-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148993953","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}