Journal of Geophysical Research: Planets最新文献

{"title":"Hydrated Silica in Oxia Planum, Mars","authors":"Joseph D. McNeil,&nbsp;Peter Grindrod,&nbsp;Livio L. Tornabene,&nbsp;Peter Fawdon,&nbsp;Vidhya Ganesh Rangarajan","doi":"10.1029/2025JE008989","DOIUrl":"https://doi.org/10.1029/2025JE008989","url":null,"abstract":"<p>Hydrated silica (SiO₂·nH₂O; opal) is important for understanding the geological and aqueous history and habitability of Mars, owing to its genesis in a wide range of aqueous environments and its high biosignature preservation potential relative to other hydrated minerals. Utilizing multispectral CaSSIS and hyperspectral CRISM data, we investigated opal-bearing deposits in Oxia Planum, the future landing site of the ExoMars “<i>Rosalind Franklin</i>” rover, in order to further assess the region's aqueous geology and astrobiological potential. Additionally, we used CaSSIS color band ratio composites to expand the CRISM data and identify discrete deposits of hydrated silica throughout the sedimentary fan stratigraphy, and identify potential opal-bearing deposits within the <i>Rosalind Franklin</i> landing ellipses. We have detected opal-bearing material in two main physiogeographic regions of Oxia Planum: (a) stratigraphically between the clay-bearing plains and the overlying sedimentary fan, and (b) in discrete outcrops in topographic lows south of the fan deposits. Amorphous opal, likely derived from weathering processes, is the dominant form of hydrated silica in Oxia Planum. Whilst a detrital origin for the hydrated silica-bearing deposits cannot be conclusively ruled out, an authigenic origin, or one in which opaline silica is concentrated by groundwater or pedogenic silicification processes, remains the most plausible formational hypotheses. These outcrops offer exciting prospects for in situ astrobiological exploration, which will allow for these hypotheses to be tested.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE008989","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145146355","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":"Classifying Thermal Moonquakes Recorded in Apollo 17 Lunar Seismic Data Using Cross-Correlation and Diurnal Temperature Variations","authors":"Y. Tamama,&nbsp;F. Civilini,&nbsp;A. Husker,&nbsp;J. M. Jackson","doi":"10.1029/2024JE008921","DOIUrl":"https://doi.org/10.1029/2024JE008921","url":null,"abstract":"<p>We refine the newly developed seismicity catalog of the Apollo 17 Lunar Seismic Profiling Experiment, containing over 12,000 thermal events, using quality control algorithms and classify these events by possible source using cross-correlation, azimuth calculation, and periodicity analysis. We first sort these events into two types—“repeating” or “isolated”—based on whether or not they share similar waveforms with at least one other event. Repeating events are characterized by minimal time between signal onset and maximum, a prevalence during early sunrise, a period consistent with the diurnal cycle, and a preferential direction to the east, coincident with the location of the Lunar Module. Isolated events, on the other hand, are distributed throughout the lunar day, originate from a wide variety of directions, and are characterized by a more gradual increase in amplitude. Many repeating events are likely caused by thermal expansion of the Lunar Module or of enclosed volatiles, while most isolated events may be caused by thermal fracturing of rock or sliding of regolith along crater slopes. In particular, we pinpoint several boulders at the Apollo 17 site whose thermally induced fractures may be the source of 45 moonquakes. Future lunar missions, such as deployments of seismic instruments or gravitational wave detectors, should be aware of thermally induced, repeating seismic signals caused by nearby boulders and structures.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145146356","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 Radiative Effect of Dust on the Convective Boundary Layer of Mars","authors":"Kun Zhang,&nbsp;Kim-Chiu Chow,&nbsp;Bowen Zhou,&nbsp;Jing Xiao","doi":"10.1029/2025JE009179","DOIUrl":"10.1029/2025JE009179","url":null,"abstract":"<p>Mars has an abundant amount of dust in its atmosphere that can have significant effects on the structure and dynamics of the Convective Boundary Layer (CBL). In this study, we employ a Large Eddy Simulation (LES) configuration of the Mars Weather Research and Forecasting (MarsWRF) model to investigate the radiative effects of dust on the Martian CBL. Our results reveal that while dust reduces the amount of solar radiation reaching the ground surface, it also absorbs and re-emits the radiation energy, leading to a warming effect in the CBL. We find that the increase in dust concentration may enhance turbulence near the top of the CBL while suppressing mixing in the lower layers. This process leads to the development of a deep but stable and stratified boundary layer, which turns out to affect the transport and distribution of dust. In addition, our results indicate that evaluating the boundary layer depth with the bulk Richardson number could be inappropriate in dusty conditions. The radiative heating of dust may reduce the vertical gradient in the Richardson number, so it is less effective to determine the true boundary layer height with the conventional threshold-based methods.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145129329","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":"Subsurface Rock Abundances in Light Plains and Ejecta Flows of the Orientale Basin","authors":"Yizhen Ma,&nbsp;Zhiyong Xiao,&nbsp;Yichen Wang,&nbsp;Wei Cao,&nbsp;Fanglu Luo,&nbsp;Rui Xu","doi":"10.1029/2025JE008938","DOIUrl":"10.1029/2025JE008938","url":null,"abstract":"<p>Smooth deposits with reflectances intermediate of basaltic mares and lunar highlands are widespread on the Moon. Termed light plains, they are mainly formed by ballistic ejecta of impact basins, and recent observations suggest that impact craters smaller than basins are also capable of forming light plains. Light plains are an important component of the lunar shallow crust, and their formation is accompanied by transportation and mixing of materials with different provenances. However, the physical properties of materials in light plains are not well constrained, but they are important to the understanding of the evolution of the lunar shallow crust. This study investigates the subsurface properties of light plains formed by the Orientale basin, and the results are compared to those of cogenetic ejecta flows (EF) formed by the Orientale basin and contemporary basaltic mare nearby. Comparison of radar scattering and thermophysical properties of these units reveals that light plains have higher abundances of centimeter- to meter-sized rock fragments. Based on the spatial distribution of fresh impact craters with and without excavated boulders, subsurface meter-sized boulder distributions are highly heterogeneous across the investigated units, with the greatest heterogeneity observed in light plains emplaced in open topography. The observations suggest that compared to the emplacement of ponded light plains and EF formed by Orientale, emplacement of the light plains in open topography was accompanied by more intense ballistic erosion of the underlying target during re-impact of melt-rich ejecta.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145110682","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":"Rock Coatings as Evidence for Late Surface Alteration on the Floor of Jezero Crater, Mars","authors":"Bradley J. Garczynski,&nbsp;Briony H. N. Horgan,&nbsp;Jeffrey R. Johnson,&nbsp;Melissa S. Rice,&nbsp;Lucia Mandon,&nbsp;Baptiste Chide,&nbsp;Andreas Bechtold,&nbsp;Pierre Beck,&nbsp;James F. Bell III,&nbsp;Erwin Dehouck,&nbsp;Alberto G. Fairén,&nbsp;Felipe Gómez,&nbsp;Pierre-Yves Meslin,&nbsp;Gerhard Paar,&nbsp;Mark A. Sephton,&nbsp;Justin I. Simon,&nbsp;Christoph Traxler,&nbsp;Alicia Vaughan,&nbsp;Roger C. Wiens,&nbsp;Tanguy Bertrand,&nbsp;Olivier Beyssac,&nbsp;Adrian J. Brown,&nbsp;Emily L. Cardarelli,&nbsp;Edward A. Cloutis,&nbsp;Louise Duflot,&nbsp;David T. Flannery,&nbsp;Patrick Gasda,&nbsp;Alexander G. Hayes,&nbsp;Christopher D. K. Herd,&nbsp;Linda Kah,&nbsp;Kjartan B. Kinch,&nbsp;Nina Lanza,&nbsp;Marco Merusi,&nbsp;Chase C. Million,&nbsp;Jorge I. Núñez,&nbsp;Ann M. Ollila,&nbsp;Clément Royer,&nbsp;Michael St. Clair,&nbsp;Christian Tate,&nbsp;Anastasia Yanchilina","doi":"10.1029/2025JE009242","DOIUrl":"10.1029/2025JE009242","url":null,"abstract":"<p>During the NASA <i>Perseverance</i> rover's exploration of the Jezero crater floor, coatings were commonly observed on rocks. These features may record past water-rock-atmosphere interactions on the crater floor, and understanding their origin is important for constraining the timing of potential water activity and habitability at Jezero. Here, we characterize the morphologic, chemical, and spectral properties of the crater floor rock coatings using color images, visible/near-infrared reflectance spectra, and chemical data from the Mastcam-Z and SuperCam instruments. We show that coatings are common and compositionally similar across the crater floor, and consistent with a mixture of dust, fine regolith, sulfates, and ferric oxides indurated as a result of one or more episodes of widespread surface alteration. All coatings exhibit a similar smooth homogenous surface with variable thickness, color, and spatial extent on rocks, likely reflecting variable oxidation and erosional expressions related to formation and/or exposure age. Coatings unconformably overlie eroded natural rock surfaces, suggesting relatively late deposition that may represent one of the last alteration episodes on the Jezero crater floor. While more common at Jezero, these coatings may be consistent with rock coatings previously observed in situ at other landing sites and may be related to duricrust formation, suggesting a global alteration process on Mars that is not unique to Jezero. The <i>Perseverance</i> rover likely sampled these rock coatings on the crater floor and the results from this study could provide important context for future investigations by the Mars Sample Return mission aimed at constraining the geologic and alteration history of Jezero crater.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009242","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145110681","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":"Two Slowly Cooled and Chemically Diverse Basalt Clasts Identified in ANGSA Core 73001","authors":"Z. E. Wilbur,&nbsp;A. N. Tatsch,&nbsp;J. J. Barnes,&nbsp;A. C. Stadermann,&nbsp;S. A. Eckley,&nbsp;T. M. Erickson,&nbsp;J. Gross,&nbsp;C. K. Shearer,&nbsp;R. A. Zeigler,&nbsp;F. M. McCubbin,&nbsp;the ANGSA Science Team","doi":"10.1029/2025JE009113","DOIUrl":"10.1029/2025JE009113","url":null,"abstract":"<p>The Apollo 17 mission returned a double drive tube, 73001/73002, which was opened after ∼50 years and made available to the community through the Apollo Next Generation Sample Analysis (ANGSA) program. Here, we investigate the petrogenesis of two basalt clasts separated from the 73001 core, samples 73001,1095B and 73001,1234B. During the preliminary examination by NASA Curation using X-ray computed tomography, these clasts were categorized as high-Ti and low-Ti basalt clasts, respectively. Our subsequent investigation confirms a high-Ti affinity for 73001,1095B, but very low-Ti (VLT) affinity for 73001,1234B. We compare 73001,1095B to other high-Ti samples and show that the basalt represents a Type1B basalt. Based on the sample's low vesicularity in 3D, coarse-grained mineralogy in 2D and 3D, and complex exsolution features, this high-Ti basalt likely cooled slowly in the thermally insulated core of a lava flow. As VLT basalts are rare or undersampled in the lunar sample collection, the investigation of 73001,1234B with 3D techniques represents the first of its kind and offers an opportunity to more robustly understand the volcanic histories of VLT lavas. We observed low vesicularity in 3D, coarse-grained mineralogy, and coarse pyroxene exsolution in the VLT basalt in agreement with previous studies suggesting that VLT basalts likely represent samples from the slowest cooled lava flows on the lunar surface, or from a shallow intrusive body. We show from the combination of 2D and 3D studies applied to small returned samples lacking geologic context that a comprehensive interpretation of their crystallization histories can be obtained.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009113","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145102111","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":"Dust Storm Influence on Gravity Wave Activity in the Nightside Thermosphere of Mars","authors":"N. B. Pickett,&nbsp;M. Felici,&nbsp;M. Mayyasi,&nbsp;P. Withers,&nbsp;M. Benna,&nbsp;S. Curry","doi":"10.1029/2025JE009171","DOIUrl":"10.1029/2025JE009171","url":null,"abstract":"<p>Gravity waves in the thermosphere of Mars are complex and variable phenomena capable of causing significant changes to processes in the upper atmosphere of Mars, which can affect atmospheric escape. The objective of this study is to determine how dust storm activity, variation in Local Solar Time (LST), and seasonal changes affect thermospheric gravity wave activity. Analyzing in situ neutral Argon density data from the Mars Atmospheric and Volatile EvolutioN (MAVEN) satellite's Neutral Gas and Ion Mass Spectrometer (NGIMS) using a new metric called Mean Integrated Wave Power (MIWP), we measure the strength of the gravity wave activity across five nightside observation data sets (each of <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 </mrow>\u0000 <annotation> ${sim} $</annotation>\u0000 </semantics></math>300 orbits) in a variety of dust conditions: three outside of the Martian Dust season with low dust conditions, one during the 2018 Global Dust Storm (GDS), and one during the regional C storm observed in Mars Year (MY) 34. During nominal, low-dust conditions, we find the MIWP metric, and thereby gravity wave activity, is twice as high post-midnight as pre-midnight. This diurnal behavior is seen here first after <i>L</i>_s = <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mn>180</mn>\u0000 <mi>°</mi>\u0000 </mrow>\u0000 <annotation> $180mathrm{{}^{circ}}$</annotation>\u0000 </semantics></math>. During the 2018 GDS, MIWP at 18:00–22:00 LST is higher when compared to dust-free conditions, consistent with past studies. However, MIWP at 22:00–06:00 LST is not statistically different from MIWP during low dust activity, suggesting that dust storm-driven variation in gravity wave activity is secondary to diurnal effects. MIWP during the MY34 regional C storm point toward 2 novel findings: seasonal variation in gravity wave activity and a strong correlation between dust loading and thermospheric gravity wave activity.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145101840","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":"A Stochastic Parameterization of Non-Orographic Gravity Waves Induced Mixing for Mars Planetary Climate Model","authors":"Jiandong Liu,&nbsp;Ehouarn Millour,&nbsp;François Forget,&nbsp;François Lott,&nbsp;Jean-Yves Chaufray","doi":"10.1029/2025JE009188","DOIUrl":"10.1029/2025JE009188","url":null,"abstract":"<p>This paper presents a formalism of mixing induced by non-orographic gravity waves (GWs) to integrate with the stochastic GWs scheme in the Mars Planetary Climate Model. We derive the formalism of GWs and their mixing under the same assumptions, integrating the two schemes within a unified framework. Specifically, a surface-to-exosphere parameterization of GW-induced turbulence has been derived in terms of the eddy diffusion coefficient. Simulations show that the coefficient is on the order of <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mn>10</mn>\u0000 <mn>4</mn>\u0000 </msup>\u0000 </mrow>\u0000 <annotation> ${10}^{4}$</annotation>\u0000 </semantics></math> to <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mn>10</mn>\u0000 <mn>9</mn>\u0000 </msup>\u0000 </mrow>\u0000 <annotation> ${10}^{9}$</annotation>\u0000 </semantics></math> <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mtext>cm</mtext>\u0000 <mn>2</mn>\u0000 </msup>\u0000 </mrow>\u0000 <annotation> ${text{cm}}^{2}$</annotation>\u0000 </semantics></math> <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mi>s</mi>\u0000 <mrow>\u0000 <mo>−</mo>\u0000 <mn>1</mn>\u0000 </mrow>\u0000 </msup>\u0000 </mrow>\u0000 <annotation> ${mathrm{s}}^{-1}$</annotation>\u0000 </semantics></math> and a turbopause is at altitudes of 70–140 km, varying with seasons. The triggered mixing has minor effects on model temperatures, yet it substantially impacts upper atmospheric abundances. Simulations are consistent with observations from the Mars Climate Sounder and the Neutral Gas and Ion Mass Spectrometer. Mixing enhances the tracer transports in the middle and upper atmosphere, governing the dynamics of these regions. The scheme reveals how non-orographic GW-induced turbulence can regulate upper atmospheric processes, such as tracer escape.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009188","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145102304","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":"Distribution of Subsurface Water in the Sulfate-Bearing Unit at Gale Crater, Mars, as Measured by the DAN Instrument on the Curiosity Rover","authors":"M. L. Litvak,&nbsp;I. G. Mitrofanov,&nbsp;M. V. Djachkova,&nbsp;D. I. Lisov,&nbsp;S. Y. Nikiforov,&nbsp;C. Hardgrove,&nbsp;A. A. Fraeman,&nbsp;B. Hallet,&nbsp;A. R. Vasavada","doi":"10.1029/2025JE009089","DOIUrl":"10.1029/2025JE009089","url":null,"abstract":"<p>The Dynamic Albedo of Neutrons (DAN) instrument onboard the Curiosity rover has been used to study subsurface water distribution in the Canaima drill site region, where polyhydrated Mg sulfate (starkeyite) was identified in Martian soil for the first time. Multiple DAN measurements acquired in this local sulfate rich area (SRA) have shown unusually high concentrations of subsurface water. The distribution of subsurface water, likely bound in sulfate minerals, is heterogeneous both laterally and with depth. 60% of the surface area around the drill site can be characterized by a layered structure, with a more hydrated, sulfate rich layer (10–30 cm) above the material that is relatively dry. These straightforward calculations suggest that the total number of Mg-sulfates in this 220 × 250 m area could be as high as 2,600 metric tons.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145101419","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 Formation of Calcium Sulfate From the Interaction Between Common Calcium-Bearing Minerals and SO2: Insights Into Mineral Stability on Venus","authors":"S. T. Port,&nbsp;D. Lukco,&nbsp;T. Kremic,&nbsp;G. W. Hunter","doi":"10.1029/2025JE009169","DOIUrl":"10.1029/2025JE009169","url":null,"abstract":"<p>The elevated surface temperature (460°C) and pressure (95 bar) on Venus, combined with the harsh gases present in the atmosphere, provide a chemically active surface environment. This study exposed three calcium-bearing minerals (calcite, anorthite, and wollastonite) to Venus's surface temperature and an atmosphere of 1.5% SO₂ in 98.5% CO₂ for three different lengths of time (6, 12, and 24 days). All three samples were coated with a continuous secondary layer of calcium sulfate within 24 days of exposure. All samples also exhibited concentrated nucleation sites on the surface, which contained larger crystals. Among the tested minerals, calcite developed the thickest layer of calcium sulfate, which is consistent with the literature, followed by wollastonite and then anorthite.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145101383","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}