Journal of Geophysical Research: Planets最新文献

{"title":"Crystallographic and Mid-Infrared Spectroscopic Properties of the CaS-MgS Solid Solution","authors":"Maximilian P. Reitze,&nbsp;Christian Renggli,&nbsp;Andreas Morlok,&nbsp;Iris Weber,&nbsp;Uta Rodehorst,&nbsp;Jasper Berndt,&nbsp;Stephan Klemme,&nbsp;Harald Hiesinger","doi":"10.1029/2024JE008483","DOIUrl":"https://doi.org/10.1029/2024JE008483","url":null,"abstract":"<p>We synthesized the solid solution between the sulfides CaS (oldhamite) and MgS (niningerite). Electron microprobe and X-ray diffraction showed homogeneous and pure samples after the synthesis. The calculated lattice parameters fit to earlier literature data. Mid-infrared spectroscopy of the samples reveal that the produced sulfides were fragile and tend to alternate very fast. However, we were able to provide clean reflectance spectra of all samples. The spectra of un-altered samples show no peaks or bands but a rather constant spectrum within the analyzed spectral range between 7.0 and 12.5 μm. The altered spectra contain signatures of sulfates and carbonates and probably further compounds. The gathered data help to understand the formation conditions of the studies sulfides as it shows that the solvus exists in the CaS-MgS system between 1000°C and 1200°C. In addition, the infrared data will help to improve remote sensing in the mid-infrared of planetary objects that might be covered with sulfide containing material like asteroids or Mercury.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 8","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-08-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008483","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141966794","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":"Experimental Constraints on the Origin of the Lunar High-Ti Basalts","authors":"C. P. Haupt,&nbsp;C. J. Renggli,&nbsp;A. Rohrbach,&nbsp;J. Berndt,&nbsp;S. Klemme","doi":"10.1029/2023JE008239","DOIUrl":"https://doi.org/10.1029/2023JE008239","url":null,"abstract":"<p>High-pressure and high-temperature experiments were conducted to simulate melting of a hybrid cumulate lunar mantle. The experimental results show that intermediate to high-Ti lunar pyroclastic glasses (&gt;6 wt% TiO₂) can be produced by partial melting of lunar cumulates. High-Ti basalts are generated when the ilmenite/clinopyroxene ratios in the lunar mantle cumulates are between 1/1 and 4/1, depending on the degree of melting. The presence of an urKREEP component in the mantle cumulate strongly influences Al₂O₃/CaO of the melts. The experiments provide strong evidence for the model that the compositional diversity of lunar basalts is a consequence of a gravitational overturn of the lunar interior after the lunar magma ocean had solidified. Ilmenite/clinopyroxene in the cumulate mantle, which generates high-Ti melts at partial melting, do not comprise the ratios in ilmenite-bearing cumulates (IBC), which crystallized after ∼90% solidification of the lunar magma ocean and indicate local accumulation of ilmenite in the overturned lunar mantle. However, to fully match the natural composition of the most primitive lunar samples, secondary processes such as assimilation are still required.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 8","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-07-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008239","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141967658","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":"Ambient Noise Tomography Reveals Asymmetric Impact Damage Zone Beneath Lonar Crater, India: Implications for Oblique Impact Cratering in Heterogeneous Basalt, With Planetary Applications","authors":"P. Sion Kumari,&nbsp;Sandeep Gupta,&nbsp;P. Senthil Kumar","doi":"10.1029/2023JE008224","DOIUrl":"https://doi.org/10.1029/2023JE008224","url":null,"abstract":"<p>Meteoroid impacts produce different types of fractures and damage zones beneath impact craters. The 3D geometry of these features reflects the trajectory and energetics of an impact event. In this study, we mapped the impact damage zone beneath the 1.88-km-diameter Lonar crater, emplaced in Deccan basalts, using Ambient Noise Tomography (ANT). A network of 23 broadband seismic stations in and around the crater yielded a 1.2 km deep 3D shear wave velocity (<i>V</i>_<i>S</i>) image covering ∼7 km by ∼5 km area. It revealed ∼500–900-m-thick heterogeneous target basalt flows, underlain by an undulating Archean granite-gneiss basement. A substantial reduction in <i>V</i>_<i>S</i> is observed beneath the crater. The original crater floor was found at a depth of 400 m below the crater rim, which is filled by impact breccia and lake sediments. Beneath the original floor, we found an oval-shaped, asymmetric 200-m-thick lensoidal low-velocity layer with a tongue-like feature beneath the southwestern ejecta blanket. The damage zone is inferred to have formed as a result of oblique impact, in which the projectile arrived from northeast to southwest direction. The <i>V</i>_<i>S</i> reduction in the low-velocity layer was used to calculate the amount of impact damage in it. The oblique impact produced a more elevated southwestern crater rim. Impact-related near-surface fracture zones up to a radial distance of &gt;1 km beneath the ejecta blanket were also found. We suggest that impact damage beneath impact craters on Earth and other planetary bodies may be imaged using ANT.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 7","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-07-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141968202","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":"Planetary-Scale Wave Activity in Venus Cloud Layer Simulated by the Venus PCM","authors":"Dexin Lai,&nbsp;Sebastien Lebonnois,&nbsp;Tao Li","doi":"10.1029/2023JE008253","DOIUrl":"10.1029/2023JE008253","url":null,"abstract":"<p>The Venus atmosphere Superrotation (SR) is successfully simulated with the high-resolution (1.25° × 1.25° in longitude and latitude) runs of the Venus Planetary Climate Model (PCM). The results show a clear spectrum and structure of atmospheric waves, primarily with periods of 5.65 and 8.5 days. The simulation reproduces long-term quasi-periodic oscillation of the zonal wind and primary planetary-scale wave seen in observations. These oscillations occur with a period of 163–222 days, although their existence is still debated in observations. The Rossby waves show similarity in wave characteristics and angular momentum (AM) transport due to Rossby-Kelvin instability by comparing the 5.65-day wave in Venus PCM with the 5.8-day wave simulated by AFES-Venus, another Venus General Circulation Model. Similarities are also evident between the 8.5-day wave in Venus PCM and the 7-day wave obtained in AFES-Venus. The long-term variations in the AM budget indicate that the 5.65-day wave is the dominant factor of the oscillation on the SR, and the 8.5-day wave plays a secondary role. When the 5.65-day wave grows, its AM and heat transport are enhanced and accelerate (decelerate) the lower-cloud equatorial jet (cloud-top mid-latitude jets). Meanwhile, the 8.5-day wave weakens, reducing its deceleration effect on the lower-cloud equator. This further suppresses the meridional gradient of the background wind and weakens instability, leading to the decay of the 5.65-day wave. And vice versa when the 5.65-day wave decays.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 7","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008253","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141845570","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":"Estimates on the Possible Annual Seismicity of Venus","authors":"Iris van Zelst,&nbsp;Julia S. Maia,&nbsp;Ana-Catalina Plesa,&nbsp;Richard Ghail,&nbsp;Moritz Spühler","doi":"10.1029/2023JE008048","DOIUrl":"10.1029/2023JE008048","url":null,"abstract":"<p>There is a growing consensus that Venus is seismically active, although its level of seismicity could be very different from that of Earth due to the lack of plate tectonics. Here, we estimate upper and lower bounds on the expected annual seismicity of Venus by scaling the seismicity of the Earth. We consider different scaling factors for different tectonic settings and account for the lower seismogenic thickness of Venus. We find that 95–296 venusquakes equal to or bigger than moment magnitude (<i>M</i>_<i>w</i>) 4 per year are expected for an inactive Venus, where the global seismicity rate is assumed to be similar to that of continental intraplate seismicity on Earth. For the active Venus scenarios, we assume that the coronae, fold belts, and rifts of Venus are currently seismically active. This results in 1,161–3,609 venusquakes ≥<i>M</i>_<i>w</i>4 annually as a realistic lower bound and 5,715–17,773 venusquakes ≥<i>M</i>_<i>w</i>4 per year as a maximum upper bound for an active Venus.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 7","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008048","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141846353","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":"Alkali Trace Elements Observed by MarSCoDe LIBS at Zhurong Landing Site on Mars: Quantitative Analysis and Its Geological Implications","authors":"Yuxuan Luo,&nbsp;Jianjun Liu,&nbsp;Zhaopeng Chen,&nbsp;Yizhong Zhang,&nbsp;Xing Wang,&nbsp;Xin Ren,&nbsp;Xiangfeng Liu,&nbsp;Zhenqiang Zhang,&nbsp;Weiming Xu,&nbsp;Rong Shu","doi":"10.1029/2024JE008366","DOIUrl":"10.1029/2024JE008366","url":null,"abstract":"<p>Mars Surface Composition Detector (MarSCoDe) is one of the important payloads carried by the Zhurong rover, China's first Mars exploration mission Tianwen-1. The laser-induced breakdown spectroscopy (LIBS) instrument of MarSCoDe is mainly used to detect major and trace elements on the surface of Mars. The quantitative analysis of alkali trace elements, namely lithium (Li), strontium (Sr), and rubidium (Rb), holds significance in unraveling the geological evolution of the Zhurong landing site. This study focuses on establishing univariate calibration models using MarSCoDe LIBS spectra from 84 samples tested in the ground laboratory. The accuracy of these models, within a few parts per million (ppm), was subsequently validated through the analysis of 12 onboard MarSCoDe Calibration Targets (MCCTs). With these models, Li, Sr, and Rb concentrations in the surface targets during the initial 300 sols (Martian days) traverse were determined. These concentrations ranged from 6 to 18, 106–628, and 22–87 ppm, respectively. Our results suggest that Li, Sr, and Rb are mainly related to the igneous rock components in the rocks and soils at the Zhurong landing site. The major secondary minerals in MarSCoDe scientific targets are likely small amounts of sulfates, which appear to have formed from the acidic weathering of recent surface brine. Clay minerals are likely either absent or very sparse in the scientific targets. The surface igneous materials at the landing site likely have originated from the most recent lava flow during the Amazonian epoch.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 7","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-07-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141851727","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 Geochemical and Mineralogical Signature of Glaciovolcanism Near Þórisjökull, Iceland, and Its Implications for Glaciovolcanism on Mars","authors":"Candice C. Bedford,&nbsp;Elizabeth B. Rampe,&nbsp;Michael T. Thorpe,&nbsp;Ryan C. Ewing,&nbsp;Kashauna Mason,&nbsp;Briony Horgan,&nbsp;Amanda Rudolph,&nbsp;Mathieu G. A. Lapôtre,&nbsp;Prakhar Sinha,&nbsp;Marion Nachon,&nbsp;Emily Champion,&nbsp;Lauren Berger,&nbsp;Ewan Reid,&nbsp;Patrick C. Gray","doi":"10.1029/2023JE008261","DOIUrl":"10.1029/2023JE008261","url":null,"abstract":"<p>Candidate glaciovolcanic landforms have been identified across Mars, suggesting that volcano-ice interactions may have been relatively widespread in areas that once contained extensive surface and near-surface ice deposits. To better constrain the detection of glaciovolcanism in Mars' geological record, this study has investigated and characterized the petrology, geochemistry, and mineralogy of three intraglacial volcanoes and an interglacial volcano in the Þórisjökull area of southwest Iceland. Our results show that glaciovolcanism creates abundant, variably altered hyaloclastite and hyalotuff that is sufficiently geochemically and mineralogically distinctive from subaerially erupted lava for identification using instruments available on Mars rovers and landers. Due to the lower gravity and atmospheric pressure at the surface of Mars, hyaloclastite and hyalotuff are also more likely to form in greater abundance in Martian glaciovolcanoes. Our results support that magmatism following deglaciation likely triggers decompression melting of the shallow mantle beneath Iceland, creating systematic changes in geochemistry and mineralogy. Glaciation can also suppress magmatism at its peak, encouraging the formation of shallow fractionated magma chambers. As such, it is possible for the crustal loading of an ice cap to enhance igneous diversity on a planet without plate tectonism, creating glass-rich, altered, and mineralogically diverse deposits such as those discovered in Gale crater by the Curiosity rover. However, as the eroded products of glaciovolcanism are similar to those formed through hydrovolcanism, the presence of a glaciovolcanic landform at the source is required to confirm whether volcano-ice interactions occurred at the sediment source.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 7","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-07-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008261","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141849637","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":"Three-Dimensional Venus Cloud Structure Simulated by a General Circulation Model","authors":"Wencheng D. Shao,&nbsp;João M. Mendonça,&nbsp;Longkang Dai","doi":"10.1029/2023JE008088","DOIUrl":"10.1029/2023JE008088","url":null,"abstract":"<p>The clouds have a great impact on Venus's energy budget and climate evolution, but its three-dimensional structure is still not well understood. Here we incorporate a simple Venus cloud physics scheme into a flexible GCM to investigate the three-dimensional cloud spatial variability. Our simulations show good agreement with observations in terms of the vertical profiles of clouds and H₂SO₄ vapor. H₂O vapor is overestimated above the clouds due to efficient transport in the cloud region. The cloud top decreases as latitude increases, qualitatively consistent with Venus Express observations. The underlying mechanism is the combination of H₂SO₄ chemical production and meridional circulation. The mixing ratios of H₂SO₄ at 50–60 km and H₂O vapors in the main cloud deck basically exhibit maxima around the equator, due to the effect of temperature's control on the saturation vapor mixing ratios of the two species. The cloud mass distribution is subject to both H₂SO₄ chemical production and dynamical transport and shows a pattern that peaks around the equator in the upper cloud while peaks at mid-high latitudes in the middle cloud. At low latitudes, H₂SO₄ and H₂O vapors, cloud mass loading and acidity show semidiurnal variations at different altitude ranges, which can be validated against future missions. Our model emphasizes the complexity of the Venus climate system and the great need for more observations and simulations to unravel its spatial variability and underlying atmospheric and/or geological processes.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 7","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-07-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008088","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141841950","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":"One Martian Year of Near-Surface Temperatures at Jezero From MEDA Measurements on Mars2020/Perseverance","authors":"A. Munguira,&nbsp;R. Hueso,&nbsp;A. Sánchez-Lavega,&nbsp;D. Toledo,&nbsp;M. de la Torre Juárez,&nbsp;A. Vicente-Retortillo,&nbsp;G. M. Martínez,&nbsp;T. Bertrand,&nbsp;T. del Rio-Gaztelurrutia,&nbsp;E. Sebastián,&nbsp;M. Lemmon,&nbsp;J. Pla-García,&nbsp;J. A. Rodríguez-Manfredi","doi":"10.1029/2024JE008385","DOIUrl":"https://doi.org/10.1029/2024JE008385","url":null,"abstract":"<p>Measurements of ground and near surface atmospheric temperatures at Jezero obtained during 700 sols by the Mars Environmental Dynamics Analyzer (MEDA) characterize the thermal behavior of the near surface Martian atmosphere during a full Martian Year. The seasonal evolution of MEDA measurements is compared with predictions from the Mars Climate Database and the solar irradiance at the surface. Thermal tides observed in the daily cycle of temperatures follow a seasonal cycle with additional variations greater than 2 K on time-scales of tens of sols. We also observe sol-to-sol variations of about 1 K in mean daily air temperatures in autumn and winter with periodicities of 4–7 sols that might be related to baroclinic disturbances that are frequent in those seasons at high latitudes. We examine the evolution of the vertical thermal gradient and temperature fluctuations without finding a seasonal response to irradiance and dust load. We find that the convective boundary layer becomes isothermal and collapses 1 hr before sunset except during northern hemisphere winter, when the collapse occurs closer to sunset, implying a longer duration of the daytime convective instability. Around this period, the rover was located in the delta front in a location of complex topography where we observed stronger thermal gradients and intense daytime air temperature fluctuations. We also find in this place a nighttime event of gravity waves on near-surface air temperatures, with amplitudes of 2 K and periods of 10 min. These waves possibly propagate downward through a near isothermal stable layer.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 7","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-07-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008385","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141736843","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":"Variable Iron Mineralogy and Redox Conditions Recorded in Ancient Rocks Measured by In Situ Visible/Near-Infrared Spectroscopy at Jezero Crater, Mars","authors":"L. Mandon,&nbsp;B. L. Ehlmann,&nbsp;R. C. Wiens,&nbsp;B. J. Garczynski,&nbsp;B. H. N. Horgan,&nbsp;T. Fouchet,&nbsp;M. Loche,&nbsp;E. Dehouck,&nbsp;P. Gasda,&nbsp;J. R. Johnson,&nbsp;A. Broz,&nbsp;J. I. Núñez,&nbsp;M. S. Rice,&nbsp;A. Vaughan,&nbsp;C. Royer,&nbsp;F. Gómez,&nbsp;A. M. Annex,&nbsp;O. Beyssac,&nbsp;O. Forni,&nbsp;A. Brown,&nbsp;J. F. Bell III,&nbsp;S. Maurice","doi":"10.1029/2023JE008254","DOIUrl":"https://doi.org/10.1029/2023JE008254","url":null,"abstract":"<p>Using relative reflectance measurements from the Mastcam-Z and SuperCam instruments on the Mars 2020 <i>Perseverance</i> rover, we assess the variability of Fe mineralogy in Noachian/Hesperian-aged rocks at Jezero crater. The results reveal diverse Fe³⁺ and Fe²⁺ minerals. The igneous crater floor, where small amounts of Fe³⁺-phyllosilicates and poorly crystalline Fe³⁺-oxyhydroxides have been reported, is spectrally similar to most oxidized basalts observed at Gusev crater. At the base of the western Jezero sedimentary fan, new spectral type points to an Fe-bearing mineral assemblage likely dominated by Fe²⁺. By contrast, most strata exposed at the fan front show signatures of Fe³⁺-oxides (mostly fine-grained crystalline hematite), Fe³⁺-sulfates (potentially copiapites), strong signatures of hydration, and among the strongest signatures of red hematite observed in situ, consistent with materials having experienced vigorous water-rock interactions and/or higher degrees of diagenesis under oxidizing conditions. The fan top strata show hydration but little to no signs of Fe oxidation likely implying that some periods of fan construction occurred either during a reduced atmosphere era or during short-lived aqueous activity of liquid water in contact with an oxidized atmosphere. We also report the discovery of alternating cm-scale bands of red and gray layers correlated with hydration and oxide variability, which has not yet been observed elsewhere on Mars. This could result from syn-depositional fluid chemistry variations, possibly as seasonal processes, or diagenetic overprint of oxidized fluids percolating through strata having variable permeability.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 7","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-07-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008254","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141736840","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}