Journal of Geophysical Research: Planets最新文献

{"title":"Thank You to Our 2024 Reviewers and Volunteers","authors":"Amanda R. Hendrix,&nbsp;Anni Määttänen,&nbsp;Laurent G. J. Montési,&nbsp;A. Deanne Rogers,&nbsp;Beatriz Sánchez-Cano,&nbsp;Bradley J. Thomson,&nbsp;Debra Buczkowski,&nbsp;Jean-Pierre Williams","doi":"10.1029/2025JE009091","DOIUrl":"https://doi.org/10.1029/2025JE009091","url":null,"abstract":"<p>At JGR: Planets, the peer review process is critical to ensuring that the published articles are based on sound scientific principles, follow state-of-the-art techniques while acknowledging relevant prior results, and present exciting discoveries or novel understanding of the fundamental processes that affect solar system objects. JGR: Planets covers a broad range of topics addressing every aspect of geoscience with the only requirement that the work addresses planetary processes. The wide breadth of topics published is reflected by our editorial team composed in 2024 of associate editors Adrian Brown, Jun Cui, Joel Davis, Leigh Fletcher, Sierra Ferguson, Yang Liu, Ananya Mallik, Germán Martínez, Anna Mittelholz, Molly McCanta, Katarina Miljkovic, Naomi Murdoch, Ryan Park, Arianna Piccialli, Laura Schaefer, Mariek Schmidt, Yasuhito Sekine, Kelsi Singer, Michael Sori, Norihiko Sugimoto, Jamey Szalay, David Trang, and Zhiyong Xiao in addition to the editors who authored this note. We rely on the expertise of the community to vet the articles submitted to the journal. In 2024, JGR: Planets benefited from 1,269 reviews provided by 816 unique volunteer referees. We also received help from organizers and guest editors working on eight active special collections. To these volunteers: We are truly grateful that you chose to dedicate your time and energy to evaluate manuscripts and to advise us on the suitability of each manuscript for JGR: Planets, often suggesting ways to improve the papers. We know that all our volunteers juggle many duties, both professional and personal. On behalf of the entire editorial board of JGR: Planets, we express our heartfelt gratitude to the many scientists who support this journal. Thank you! You are performing a valued service to this journal and to the community.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 4","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009091","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143717076","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":"Characterizing Inter-Annual and Inter-Seasonal Dust Deposition and Removal on Mars Using Thermal Emission Imaging System (THEMIS) Infrared Data","authors":"C. A. Wolfe,&nbsp;C. S. Edwards,&nbsp;S. Piqueux","doi":"10.1029/2024JE008470","DOIUrl":"https://doi.org/10.1029/2024JE008470","url":null,"abstract":"<p>The current climate of Mars is characterized by frequent dust storms, during which dust is raised from the surface and transported throughout the atmosphere via global circulation and wind patterns. The addition or removal of dust can cause the surface to brighten or darken significantly. This process not only modifies the appearance of the surface, but alters the thermal insulation properties due to the low thermal conductivity of dust. Of particular interest is the inter-annual/seasonal pattern of dust redistribution and the spatial scales at which such process take place. While global climate models predict changes in surface dust coverage before and after global storms, their output concerning the amount and locations of transported dust differs significantly. Changes in both dust coverage and thickness are constrained by employing a numerical thermal model and analyzing surface temperature differences from overlapping Thermal Emission Imaging System-Infrared images. A multi-dimensional lookup table relating thermal inertia, surface temperature difference, and dust layer thickness is constructed to derive changes in surface dust redistribution at high spatial resolution for both inter-annual/seasonal timescales. Modeled surface albedos are also derived to provide an additional constraint on surface dust redistribution. Upper and lower limits for derived changes in surface dust thickness are established from variations in surface temperature and modeled surface albedo respectively. Upon analyzing two distinct image pairs, we find that dust deposition/removal can occur at small spatial scales (i.e., 100s of m) and that changes in surface dust thickness can range from a few to hundreds of microns.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143689924","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":"Characteristics of Space Weathering Modification of Chang'e-5 Lunar Soil: Evidence From the Microanalysis of Anorthite","authors":"Ronghua Pang,&nbsp;Zhuang Guo,&nbsp;Chen Li,&nbsp;Sizhe Zhao,&nbsp;Xiongyao Li,&nbsp;Yuanyun Wen,&nbsp;Shuangyu Wang,&nbsp;Rui Li,&nbsp;Yang Li","doi":"10.1029/2024JE008611","DOIUrl":"https://doi.org/10.1029/2024JE008611","url":null,"abstract":"<p>Due to the lack of an atmosphere and a global magnetic field on the Moon, its surface is extensively subject to space weathering. One of the important products of space weathering is the iron particle, which has significant impacts for planetary exploration. Research on Apollo samples suggests that iron particles primarily form through vapor deposition processes during meteorite impacts. The Chang'e-5 (CE5) samples are the youngest samples collected so far, and the phenomenon of surface vapor deposition has not been studied in depth. Anorthite stoichiometrically free of Fe minerals, is highly suitable for studying the vapor deposition process of iron particles. Five anorthite grains from CE5 were analyzed using transmission electron microscope (TEM). Results show that the iron particle on the surface of anorthite formed from impact sputtering glass, and lack vapor-deposited nanophase iron particles (np-Fe⁰, &lt;100 nm) on its surface. Additionally, residual Fe from Fe-Mg silicate impactors on the anorthite surface did not form np-Fe⁰. The dominant mechanism of np-Fe⁰ formation due to space weathering differs between the CE5 and Apollo landing sites. Impact melting rather than vapor deposition may be the dominant mechanism of np-Fe⁰ formation at the CE5 landing site due to impact. This indicates that the meteorite impact environment of CE5 landing site is weak. It is not possible to generate a large amount of vapor deposition-derived np-Fe⁰ like in Apollo samples.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143689596","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":"Numerical Simulation of Martian Ionospheric Irregularities","authors":"Konghan Jiang,&nbsp;Jiuhou Lei,&nbsp;Maodong Yan,&nbsp;Binzheng Zhang","doi":"10.1029/2024JE008898","DOIUrl":"https://doi.org/10.1029/2024JE008898","url":null,"abstract":"<p>Martian ionospheric irregularities have been observed via Mars Atmosphere and Volatile EvolutioN (MAVEN) in situ measurements, but their generation mechanism is still unclear. In this work, we develop a two-dimensional model to investigate the formation of Martian irregularities. Both the simulation results and linear theory indicate that Martian ionospheric irregularities can be triggered by the Rayleigh-Taylor instability. Unlike at Earth, the irregularity at Mars strongly depends on the wavelength of perturbation. It is found that the large Hall conductivity (Hall current) at the Martian ionosphere is the cause of the complex irregularity structures, especially for long wavelength perturbations. Specifically, the Hall current leading to tilt transport of plasma disrupts the initial perturbation waves, and thus results in the formation of multiple small irregularity structures from non-linear process.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143689597","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":"Martian Smectites Formation Regulated by Environmental CO2 and Si","authors":"Tianqi Zhang,&nbsp;Qi Tao,&nbsp;Xiaorong Qin,&nbsp;Yuchun Wu,&nbsp;Jiaxin Xi,&nbsp;Xiaoliang Liang,&nbsp;Hongping He,&nbsp;Sridhar Komarneni","doi":"10.1029/2024JE008619","DOIUrl":"https://doi.org/10.1029/2024JE008619","url":null,"abstract":"<p>Despite the anticipated abundant carbonates due to historical atmospheric CO₂ levels, Mars presents a geological puzzle with MgFe-smectites dominating the Noachian and early Hesperian terrains, contrasted by sparse carbonate deposits. To address this point, we explored the impact of CO₂ on MgFe-smectite formation, emphasizing the role of variable Si concentrations within the simulated Martian environment. Hydrothermal experiments, conducted under a constant CO₂ concentration (C0.5) and varying Si concentrations (Si0.5 to Si4), reveal a transformation from pyroaurite to MgFe-smectite via lizardite as an intermediary phase. This transformation underscores the crucial role of Si in this mineral sequence. Notably, experiments demonstrate that the interlayer CO₃²⁻ in pyroaurite is released into aqueous environments during the mineral conversion, potentially impacting the Martian CO₂ budget. These findings could explain isolated carbonate outcrops and the possibility of hydrotalcite-group minerals on Mars today. Further Mars exploration should consider identifying hydrotalcite-group minerals for their implications on the planet's climate and habitability.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143689212","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":"Slopes of Lunar Crater Size-Frequency Distributions on Exterior Impact Melt Deposits of Young Craters","authors":"A. Oetting,&nbsp;W. Iqbal,&nbsp;N. Schmedemann,&nbsp;G. Michael,&nbsp;H. Hiesinger,&nbsp;C. H. van der Bogert,&nbsp;T. Heyer","doi":"10.1029/2024JE008589","DOIUrl":"https://doi.org/10.1029/2024JE008589","url":null,"abstract":"<p>Lunar impact craters can be used as a tool to derive information about the timing and sequence of the emplacement of geologic units and surface processes on the Moon. The production function (PF) derived from crater size-frequency distribution (CSFD) measurements is an essential component in determining the model age of a geologic surface. The PFs of Neukum (1983) and Neukum et al. (2001), https://doi.org/10.1007/978-94-017-1035-0_3 are defined only over a crater diameter range between 10 m and 300 km and are among the most frequently used PFs. However, a potential extension of the valid crater diameter range to smaller craters may be possible due to the availability of high-resolution image data, and a larger number of small craters could reduce the statistical errors in age determinations. To evaluate whether CSFD measurements with craters ≤10 m are suitable for inclusion in a PF, we complement the investigation of ejecta blankets (Oetting et al., 2023, https://doi.org/10.1029/2023je007816) by analyzing the CSFD slopes of small craters formed on impact melt deposits of young Copernican-aged craters Tharp, Korolev Z, Thales, and Glushko. The resulting CSFD slopes are slightly steeper for craters between 10 and 20 m than the proposed cumulative −3 slopes by Neukum (1983) and Neukum et al. (2001), https://doi.org/10.1007/978-94-017-1035-0_3. The CSFD slope for craters ≤10 m is shallower than −3. In this study, the CSFD slopes are derived from unbinned data, but we present our CSFD measurements in both unbinned and binned form. Our results indicate that small crater diameters (≤10 m) can be included for extending a PF.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008589","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143689342","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":"Meridional Distribution of CO, H2O, and H2SO4 in the Venus' Atmosphere: A Two-Dimensional Model Incorporating Transport and Chemical Reaction","authors":"Shinya Kuwayama,&nbsp;George L. Hashimoto","doi":"10.1029/2024JE008596","DOIUrl":"https://doi.org/10.1029/2024JE008596","url":null,"abstract":"&lt;p&gt;We developed a 2-dimensional model of Venus' atmosphere which calculates meridional distributions of chemical species such as CO, &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msub&gt;\u0000 &lt;mi&gt;H&lt;/mi&gt;\u0000 &lt;mn&gt;2&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; ${mathrm{H}}_{2}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;O, and &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msub&gt;\u0000 &lt;mi&gt;H&lt;/mi&gt;\u0000 &lt;mn&gt;2&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;msub&gt;\u0000 &lt;mtext&gt;SO&lt;/mtext&gt;\u0000 &lt;mn&gt;4&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; ${mathrm{H}}_{2}{text{SO}}_{4}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;. To calculate the meridional distribution of chemically active species, we combined chemical model, cloud model, and transport model. Partitioning between gas and liquid phase is calculated assuming vapor-liquid equilibrium, and the number density of cloud droplet is calculated by taking coagulation into account. Our model demonstrated that the meridional distributions of CO and &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msub&gt;\u0000 &lt;mi&gt;H&lt;/mi&gt;\u0000 &lt;mn&gt;2&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; ${mathrm{H}}_{2}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;O are sensitive to the circulation of the Venus' atmosphere. Observed meridional distribution of CO indicates that there is a large scale meridional circulation from the lower (below 20 km altitude) to the upper (around 80 km altitude) atmosphere. Also observed concentration of &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msub&gt;\u0000 &lt;mi&gt;H&lt;/mi&gt;\u0000 &lt;mn&gt;2&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; ${mathrm{H}}_{2}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;O vapor above the cloud top suggests that meridional circulation ventilates the air above the cloud top on a time scale of 600 days. In our model, thick clouds at low latitudes are maintained by meridional circulation, while thick clouds at high latitudes are caused by latitudinal temperature gradient and horizontal transport of &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msub&gt;\u0000 &lt;mi&gt;H&lt;/mi&gt;\u0000 &lt;mn&gt;2&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;msub&gt;\u0000 &lt;mtext&gt;SO&lt;/mtext&gt;\u0000 &lt;mn&gt;4&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; ${mathrm{H}}_{2}{text{SO}}_{4}$&lt;/annotation&gt;\u0000","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008596","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143689077","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":"Detectability of Coastal Landforms on Titan With the Cassini RADAR","authors":"S. P. D. Birch,&nbsp;R. V. Palermo,&nbsp;U. G. Schneck,&nbsp;A. Ashton,&nbsp;A. G. Hayes,&nbsp;J. M. Soderblom,&nbsp;W. H. Mitchell,&nbsp;J. T. Perron","doi":"10.1029/2024JE008737","DOIUrl":"https://doi.org/10.1029/2024JE008737","url":null,"abstract":"<p>Earth's coastlines serve as the intersection for numerous physical and chemical processes between terrestrial and marine systems. Liquids of different compositions meet, materials eroded from the continents are concentrated in sedimentary deposits, and the diverse planform morphologies of coastal landforms are shaped by erosional and sediment transport processes. Accordingly, coastal landscapes preserve valuable records of processes that govern Earth's climate, materials, and tectonic history. Applying our understanding from Earth to the coastlines around Titan's liquid hydrocarbon seas allows us to investigate the climate history of the only other known active hydrological system. The study of Titan's coastlines, particularly its deltas, however, remains challenging due to the limitations of Cassini Synthetic Aperture Radar (SAR) data and the transparency of Titan's fluids to microwave radiation. To understand these limitations, we developed a numerical model to simulate Earth's coastlines as they would appear in Cassini SAR images. We show that multi-kilometer-scale landforms are detectable on Titan, provided there is sufficient contrast between the land surface and seafloor. We revisit Titan and show that many of its large coastal rivers do not terminate in deltas, in contrast to Earth. Additionally, we uncover submerged features on Titan's seafloors, suggesting sea-level cycling and/or active sub-aqueous flow. We propose preliminary hypotheses to explain the presence or absence of various coastal landforms on Titan, offering directions for future investigations into Titan's climate and materials. Moreover, we emphasize the opportunities and benefits a superior imaging system at Titan could provide to both Titan science and studies of Earth's changing coasts.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143689076","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":"Martian Highlands Differentiation Concomitant to Dichotomy Formation","authors":"Valentin Bonnet Gibet,&nbsp;Chloé Michaut,&nbsp;Thomas Bodin,&nbsp;Mark Wieczorek,&nbsp;Fabien Dubuffet","doi":"10.1029/2024JE008486","DOIUrl":"https://doi.org/10.1029/2024JE008486","url":null,"abstract":"<p>The Martian surface composition appears mainly mafic but recent observations have revealed the presence of differentiated rocks, only in the highlands. Here, we demonstrate that differentiated melts can form during the construction of thick crustal regions on Mars by fractional crystallisation of a mafic magma, without plate tectonics. On a stagnant-lid planet, regions of thicker crusts contain more heat-producing elements and are associated to thinner lithospheres and to higher mantle melt fractions. This induces larger crustal extraction rates where the crust is thicker. This positive feedback mechanism is favored at large wavelengths and can explain the formation of the Martian dichotomy. We further develop an asymmetric parameterized thermal evolution model accounting for crustal extraction, where the well-mixed convective mantle is topped by two lithospheres (north/south) characterized by specific thermal and crustal structures. We use this model in a Bayesian inversion to investigate the conditions that allow crustal temperatures to be maintained above the basalt solidus during crustal growth, resulting in the formation of evolved melts. Among the thermal evolution models matching constraints on the structure of the Martian crust and mantle provided by the InSight NASA mission, a non-negligible fraction allows partial melting and differentiation of the crust in the south, which can occur very early (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>&lt;</mo>\u0000 </mrow>\u0000 <annotation> ${&lt; } $</annotation>\u0000 </semantics></math>100 Myr) as well as during the Hesperian; partial melting in the north appears unlikely. Although crustal differentiation may occur on a hemispheric scale on Mars, its vertical extent would be limited to less than a third of the crustal thickness.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008486","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143689078","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":"Metal Limiting Habitability in Enceladus? Availability of Trace Metals for Methanogenic Life in Hydrothermal Fluids","authors":"Shuya Tan,&nbsp;Yasuhito Sekine,&nbsp;Takazo Shibuya","doi":"10.1029/2024JE008591","DOIUrl":"https://doi.org/10.1029/2024JE008591","url":null,"abstract":"<p>Enceladus' ocean could support methanogenic life in terms of the availability of chemical energy (H₂ and CO₂) and nutrients (N and P). However, excess energy and nutrients in the ocean raise the question of why they remain abundant if Enceladus is inhabited. Terrestrial methanogens require trace metals, such as Co, Ni, Cu, Zn, and Mo, for their enzyme activation; nevertheless, the availability of these trace metals is largely unknown in Enceladus' ocean. Here, we investigate concentrations of dissolved trace metals in Enceladus based on hydrothermal experiments and thermodynamic equilibrium calculations in order to understand the minerals that control their concentrations in water-rock interactions. Our results show that Ni and Co concentrations in hydrothermal fluids can be controlled by dissolution of a sulfide mineral, pentlandite, in chondritic rocks. In a pH range for Enceladus' ocean, our calculations show that hydrothermal environments would be the source of dissolved Ni and Co. Given a suggested range of water chemistry (pH and dissolved species) of Enceladus' ocean, Ni, Zn, and Mo concentrations in hydrothermal fluids would be comparable to the levels required for terrestrial methanogens. However, both Co and Cu concentrations would be depleted compared with the levels required for terrestrial methanogens. We suggest that if methanogenic life in Enceladus requires trace metals at the same levels as for terrestrial methanogens, the availability of Co and Cu could control the activity of methanogenesis, possibly leaving excess chemical energy and nutrients in the ocean.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008591","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143646259","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}