Journal of Geophysical Research: Planets最新文献

{"title":"Titan's Lithospheric Strength Envelope and Brittle–Ductile Transition: The Importance of Crustal Pore Fluids, Organics, and Clathrates","authors":"L. R. Schurmeier,&nbsp;S. A. Fagents","doi":"10.1029/2025JE009118","DOIUrl":"10.1029/2025JE009118","url":null,"abstract":"<p>The strength and thickness of Titan's lithosphere is likely influenced by its unique organic-rich crust. Titan's crust may be composed of water ice or a more insulating layer of methane clathrate (MC), and topped by potentially insulating surface deposits such as sand, labyrinth terrains, undifferentiated plains, and methane/ethane seas and pore fluids. We investigate the thermal and mechanical influences of potential crustal materials on Titan's lithosphere. We present a suite of lithospheric strength envelopes using two strain rates and three ice grain sizes to calculate the brittle–ductile transition depth, the thickness of the brittle lithosphere. We found that the brittle lithosphere could be as thin as 3–5 km for the thinnest MC crust cases explored (5 and 10 km thick crusts, respectively). A clathrate-free ice shell could have a lithosphere as thin as 10–12 km when convecting, or 20–26 km without convection, depending on the assumed heat flow. Highly insulating surface layers could thin the local lithosphere by a few kilometers. Generally, Titan's lithosphere is strong, of order a few MPa near the surface to &gt;100 MPa at depth for the thermal profiles explored. When pore fluid pressure is considered, the stress required for brittle failure can be reduced to &lt;1 MPa near the surface. To form the observed mountains via tidal stresses (of order 10s kPa), we suggest that a combination of crustal properties co-occur, which locally weakens the lithosphere and focuses stress.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145021988","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":"Endogenous, yet Exotic, Sulfur in the Lunar Mantle","authors":"J. W. Dottin III,&nbsp;S. B. Simon,&nbsp;C. K. Shearer,&nbsp;J. Benson,&nbsp;H. Fu,&nbsp;J. S. Boesenberg,&nbsp;B. Monteleone,&nbsp;the ANGSA Science Team","doi":"10.1029/2024JE008834","DOIUrl":"10.1029/2024JE008834","url":null,"abstract":"<p>In situ sulfur isotope analyses of sulfides found in regolith particles from the recently opened Apollo 17 drive tube 73001/2 reveal variable ³⁴S/³²S and ³³S/³²S that range from that of typical lunar basalts to strongly ³⁴S- and ³³S-depleted values (δ³⁴S = −4.1 ± 0.35 to +1.5 ± 0.029; Δ³³S = −2.8 ± 0.48 to −0.1 ± 0.27 (2σ)). All Δ³³S and δ³⁴S data are positively correlated. The correlation indicates mixing between at least two distinct sources of sulfur in the lunar mantle, one of which is associated with photochemically processed sulfur from a gaseous environment (strongly negative Δ³³S). The gaseous precursor and its preservation in endogenous sulfides require that either the sulfur was delivered to the lunar mantle early in its history through unknown processes or it is a remnant of the giant Moon-forming impactor.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145021989","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":"Vertical Propagation of Venusian Thermal Tides Above and Below Clouds Revealed by Akatsuki Radio Occultation","authors":"Hiroki Ando,&nbsp;Katsuyuki Noguchi,&nbsp;Takeshi Imamura,&nbsp;Masahiro Takagi,&nbsp;Norihiko Sugimoto,&nbsp;Yoshihisa Matsuda,&nbsp;Silvia Tellmann,&nbsp;Martin Pätzold,&nbsp;Bernd Häusler,&nbsp;Raj Kumar Choudhary,&nbsp;Maria Antonita","doi":"10.1029/2025JE009165","DOIUrl":"10.1029/2025JE009165","url":null,"abstract":"<p>The vertical structure of the thermal tide in the Venusian low-latitude region (0<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>°</mo>\u0000 </mrow>\u0000 <annotation> ${}^{circ}$</annotation>\u0000 </semantics></math>–30<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>°</mo>\u0000 </mrow>\u0000 <annotation> ${}^{circ}$</annotation>\u0000 </semantics></math> latitudes) was investigated by the Akatsuki radio occultation measurements. The result shows that the phase of the diurnal tide little varies in the vertical direction, while that of the semidiurnal tide tilts toward earlier local times with increasing altitude above 65 km and tilts in the same direction with decreasing altitude below 50 km. This indicates that the semidiurnal tide is excited between 50 and 65 km altitudes and propagates upward above these heights and downward below. The vertical momentum flux associated with the semidiurnal tide in low latitudes was calculated above 58 km, and the associated acceleration rate was estimated to be <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 </mrow>\u0000 <annotation> ${sim} $</annotation>\u0000 </semantics></math>0.30 m <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> <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mtext>day</mtext>\u0000 <mrow>\u0000 <mo>−</mo>\u0000 <mn>1</mn>\u0000 </mrow>\u0000 </msup>\u0000 </mrow>\u0000 <annotation> ${text{day}}^{-1}$</annotation>\u0000 </semantics></math> near the cloud top, which is comparable to those expected in the previous numerical studies. Our results observationally confirmed the simultaneous upward and downward propagations of the thermal tide, which can account for the vertical shear of the Venusian atmospheric superrotation in low latitudes, supporting the previous theoretical predictions.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145012860","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":"Northwest Africa 16788: The Largest Known Individual Martian Meteorite—A New Olivine Microgabbroic Shergottite and Its Implications for Martian Magmatism","authors":"Xhonatan Shehaj,&nbsp;Giovanni Pratesi,&nbsp;Cristian Carli,&nbsp;Riccardo Avanzinelli,&nbsp;Alice Stephant,&nbsp;Annarita Franza,&nbsp;Eleonora Ammannito","doi":"10.1029/2024JE008885","DOIUrl":"10.1029/2024JE008885","url":null,"abstract":"<p>We present a comprehensive study of a new Martian meteorite, Northwest Africa (NWA) 16788, found in the Sahara Desert in July 2023. This specimen constitutes the largest known individual meteorite of Martian origin, with a total weight of ⁓25 kg. A detailed mineralogical and geochemical investigation identifies NWA 16788 as an enriched olivine microgabbroic shergottite. Petrographic analysis reveals a millimeter-sized cumulate texture, which is intermediate between poikilitic and gabbroic shergottites, primarily composed of pyroxene (⁓61 vol.%), maskelynite (shocked plagioclase, ⁓21 vol.%), and olivine (⁓15 vol.%). Pyroxene grains exhibit a distinctive zoning pattern, placing NWA 16788 within a small group of Martian meteorites and lunar samples that record unique cooling histories, suggesting that similar samples may be more prevalent within the Martian igneous rocks than previously recognized. High-precision analyses of bulk ¹⁴³Nd/¹⁴⁴Nd and ⁸⁷Sr/⁸⁶Sr isotopic composition, combined with trace element abundance, indicate that NWA 16788 originated from the partial melting of an enriched Martian mantle source. Electron backscatter diffraction analysis reveals a unimodal distribution of olivine grain misorientation, averaging ⁓4.6°, consistent with a high-energy single-impact event. Moreover, visible and near-infrared spectroscopy data acquired on NWA 16788 could aid in identifying potential locations of analogous igneous rocks on the Martian surface. Finally, this study proposes refinements to the current classification scheme of Martian meteorites, aiming to reduce taxonomic ambiguity and improve the alignment between Martian meteorites and Martian igneous rocks, based on data from Mars rovers.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008885","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145005600","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":"Martian High-Frequency Gravity Waves Observed by Zhurong and Perseverance Rovers Before and After a Regional Dust Storm","authors":"Chengyun Yang,&nbsp;Cong Sun,&nbsp;Chao Ban,&nbsp;Dexin Lai,&nbsp;Zhaopeng Wu,&nbsp;Xin Fang,&nbsp;Jun Yang,&nbsp;Yongyun Hu,&nbsp;Tao Li","doi":"10.1029/2025JE009022","DOIUrl":"10.1029/2025JE009022","url":null,"abstract":"<p>This study investigated high-frequency gravity waves (HFGWs) with periods below 20 min observed by the Zhurong/Tianwen-1 and Perseverance/Mars 2020 rovers between local time 09:00 and 11:00, from Ls 140°–165° in Mars Year 36. By analyzing the eccentricity of monochromatic wind perturbations in the horizontal wind data, HFGWs were identified via their predominantly linear characteristics in hodographs. The propagation directions of these waves were determined using polarization relationships from the linear theory of HFGWs. The occurrence of HFGWs doubled following the onset of a regional dust storm in the Utopia Planitia where the Zhurong rover landed. The HFGWs observed by Zhurong predominantly propagated in a north-south direction before the dust storm and then shifted into an east–west direction afterward. In this study, the temperature and wind simulations from the Mars Planetary Climate Model were used to estimate atmospheric instability by calculating the Richardson number before and after the dust storm in the locations of both rovers. As the dust storm developed, intensified dust fronts moved northward from the tropical region and modulated atmospheric instability to the south of Zhurong, which may be responsible for the decrease in wave propagation along the north-south direction.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145005589","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":"Abundant Non-Mare Components in the Chang'e-6 Lunar Regolith: Constraints From Plagioclase Fragments and Impact Glasses","authors":"Zhiming Chen,&nbsp;Le Zhang,&nbsp;Jingyou Chen,&nbsp;Chngyuan Wang,&nbsp;Jintuan Wang,&nbsp;Zexian Cui,&nbsp;Zuyang Zou,&nbsp;Pengli He,&nbsp;Yonghua Cao,&nbsp;Qin Zhou,&nbsp;Linli Chen,&nbsp;Yan-Qiang Zhang,&nbsp;Yi-Gang Xu","doi":"10.1029/2025JE008976","DOIUrl":"10.1029/2025JE008976","url":null,"abstract":"<p>Lunar regolith contains not only materials derived from the local rock unit, but also materials transferred from remote craters, which are crucial for investigating the lithological diversity of the lunar surface. In this study, we conducted detailed petrography and geochemical analyses and measured the cross-sectional area of plagioclase fragments and impact glass particles selected from the Chang'e 6 (CE-6) regolith, the first lunar far-side returned sample. Statistics of plagioclase fragments and impact glass are used to estimate the proportion of the diverse components in the CE-6 regolith. The results reveal 35.7 vol% and 28.2 vol% exotic components in CE-6 plagioclase and impact glass fractions, respectively. As plagioclase, pyroxene and glass particles are the three dominant phases (&gt;95 vol%) in the CE-6 regolith, together with previously reported pyroxene compositions, we estimate that the abundance of the exotic materials is 23.5–33.5 vol%. These exogeneous components include very-low-Ti (VLT) basalt (2%–3%), ferroan anorthosite (5%–9%), Mg-suite (15%–20%), KREEP-related (∼0.1%), and highlands-mare-mixed materials (∼1%). The VLT-basalt component is most likely from the mare basalt unit to the east of the landing site or beneath the local mare layer. Based on the ejecta orientations and model age of impact craters, ferroan anorthite, Mg-suite and KREEP-related materials are likely transferred from Vavilov/Pythagoras (highland anorthosite), Chaffee S/White’ (rich in mafic minerals), and Birkeland (high Th contents) craters, respectively. The abundant non-mare components in the CE-6 regolith contrast to the very scarce exotic materials in the CE-5 lunar regolith, potentially providing valuable insights into the composition of the lunar far-side.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144998616","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 Effect of Near-Surface Winds on Surface Temperature and Dust Transport on Venus","authors":"Maxence Lefèvre,&nbsp;Sébastien Lebonnois,&nbsp;Aymeric Spiga,&nbsp;François Forget","doi":"10.1029/2025JE009133","DOIUrl":"10.1029/2025JE009133","url":null,"abstract":"<p>The knowledge of the Venus near-surface atmosphere is sparse. Few spacecrafts landed on the surface and measured winds with amplitudes below 1 m/s. The diurnal cycle of the wind amplitude and orientation is not known. Recent numerical simulations showed that slope winds along topographic structures could strongly impact the direction of winds. This study presents the first mesoscale modeling of such winds on Venus. A change of direction is occurring during the day in the main slopes, with upslope winds at noon due to solar heating and downslope winds at night. This is due to efficient IR cooling of the surface during the night, being colder than its surroundings slope atmospheric environment and leading to displacement of air. The temperature is impacted by the adiabatic cooling/warming induced by those winds. A strong heating effect is occurring for the downslope winds, leading to an anti-correlation between the surface temperature diurnal amplitude and the topography. This diurnal amplitude reaches 4 K in the plains and below 1 K in the mountains. The saltation of sediment by those winds was also quantified, with a higher probability at night along the slopes on the western flanks.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009133","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144998635","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Many Fates of Pluto's Subsurface Ocean","authors":"Julia Miller,&nbsp;Elodie Lesage,&nbsp;Samuel Howell,&nbsp;Samuel Birch","doi":"10.1029/2025JE009120","DOIUrl":"10.1029/2025JE009120","url":null,"abstract":"<p>A continuously increasing number of objects in our solar system have been classified as “ocean worlds,” harboring recent or past subsurface oceans of liquid water. These discoveries raise the potential of persistent habitability even in the frigid environments of the outer solar system. The presence of subsurface oceans within the largest and most tidally dissipative icy moons is consistent with the current understanding of their heat budgets, but suggestions of present-day oceans within smaller moons and Kuiper Belt Objects are harder to reconcile with simple thermal evolution models. It has been suggested that a methane clathrate layer within Pluto's shell would insulate a subsurface ocean and extend its lifetime. However, insulating effects have not been considered in the context of an ice shell experiencing solid-state convection, a key geodynamic process for ocean world evolution. We have therefore developed a 1-Dimensional (1D) thermal evolution model for an icy body with a time-evolving ice shell composition, to investigate the effects of basal methane clathrate incorporation on convective vigor and interior evolution. We apply our model to Pluto, a mid-sized icy world with relatively few complicating factors. We find that the addition of methane clathrate to a convecting ice shell can result in complex feedback mechanisms, causing nonlinear variation in maximum ocean thickness and temperature. This work takes a first step toward understanding both the thermal evolution of, and material transport within, compositionally complex ice shells. These results have implications for the longevity of subsurface oceans and the related habitability of these worlds.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144998780","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":"Magnetic Mineralogy in Lunar Mare Basalts and Implications for Paleointensity Retrieval","authors":"Ji-In Jung,&nbsp;Sonia M. Tikoo,&nbsp;Zoltán Váci,&nbsp;Michael J. Krawczynski,&nbsp;Peat Solheid,&nbsp;Dale H. Burns,&nbsp;Arturas Vailionis","doi":"10.1029/2025JE009030","DOIUrl":"10.1029/2025JE009030","url":null,"abstract":"<p>Lunar paleomagnetic studies have identified multidomain metallic Fe–Ni alloys as the dominant magnetic contributors in mare basalts. Here, we explore the low-temperature magnetic behavior of standard samples for a suite of opaque minerals that occur within mare basalts (single-domain and multidomain Fe, wüstite, ulvöspinel, iron chromite, ilmenite, and troilite). We compare the observed low-temperature behaviors to those of several Apollo mare basalt samples (10003, 10044, 10020, 10069, 10071, 12009, 12022, 15597). Notable magnetic transitions were detected at <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>&lt;</mo>\u0000 </mrow>\u0000 <annotation> ${&lt; } $</annotation>\u0000 </semantics></math>30 K (ilmenite), 60–80 K (chromite, troilite), and 100–125 K (ulvöspinel, chromite). We also investigated the effects of low-temperature cycling on mare basalt remanence and observed that only grains with coercivities <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>&lt;</mo>\u0000 </mrow>\u0000 <annotation> ${&lt; } $</annotation>\u0000 </semantics></math>20–40 mT were cleaned. This suggests a minimal impact of diurnal temperature cycling at the lunar surface on the retrieved lunar paleointensity values. Using comprehensive electron microscopy techniques, including scanning electron microscopy (SEM), energy dispersive spectroscopy (EDS), wavelength dispersive spectroscopy (WDS), x-ray diffraction, and transmission electron microscopy (TEM), we further examined magnetic phases within four Apollo 11 mare basalt samples. Our findings revealed the presence of Fe grains (one to 10 μm in diameter) associated with troilite contain sub-grains ranging in size from tens to hundreds of nanometers in some samples. These grains, which fall within the single-domain to multi-domain range as observed in their first-order reversal curves, might have the potential to retain high coercivity components and thereby effectively record an ancient dynamo field.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JE009030","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144929705","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":"A Comprehensive Framework for Assessing Terrestrial Analogue Field Sites for Ocean Worlds","authors":"Jennifer C. Stern,&nbsp;Heather V. Graham,&nbsp;Bradley Burcar,&nbsp;Emily S. Martin,&nbsp;Aaron Noell,&nbsp;Kevin Hand,&nbsp;Jeff S. Bowman,&nbsp;Peter Doran,&nbsp;Virginia Edgcomb,&nbsp;James F. Holden,&nbsp;Alta E. G. Howells,&nbsp;Michael J. Malaska,&nbsp;Brook L. Nunn,&nbsp;Jani Radebaugh,&nbsp;Laura E. Rodriguez,&nbsp;Schuyler Borges,&nbsp;Dina Bower,&nbsp;Samuel Courville,&nbsp;Melisa Diaz,&nbsp;Benjamin Hockman,&nbsp;Julie Huber,&nbsp;Justin Lawrence,&nbsp;Trista Vick-Majors,&nbsp;Conor A. Nixon,&nbsp;John R. Spear,&nbsp;Amanda V. Steckel,&nbsp;Anezina Solomonidou,&nbsp;Nicholas Schmerr,&nbsp;Britney Schmidt,&nbsp;Matthew O. Schrenk,&nbsp;Lauren Seyler,&nbsp;Amy R. Smith,&nbsp;Catherine C. Walker,&nbsp;Patrick Whelley,&nbsp;Natalie Wolfenbarger,&nbsp;Steven D. Vance","doi":"10.1029/2024JE008803","DOIUrl":"10.1029/2024JE008803","url":null,"abstract":"<p>Field studies at terrestrial analogue sites represent an important contribution to the science of ocean worlds. The value of the science and technology investigations conducted at field analogue sites depends on the relevance of the analogue environment to the target ocean world. We accept that there are no perfect analogues for many of the unique environments represented by ocean worlds but suggest that a one-to-one matching of environmental characteristics and conditions is not crucial to the success or impact of the work. Instead, we must determine which processes and parameters are required to map directly to the target ocean world environment with high fidelity to address the science question. In this review paper, we discuss the outcomes of a workshop aimed at developing a new framework for evaluating the suitability of analogue field locations for ocean worlds research. Here we present a two-step approach to (a) identify the most crucial processes and parameters associated with a given science question and (b) assess the fidelity of these processes and parameters at a proposed field site to those expected for the target ocean world. We demonstrate this approach in a test case evaluating three types of ocean world analogue environments with respect to a science question. The consensus document presented here equips veteran and new investigators with valuable tools to better assess and justify their analogue site selections.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 9","pages":""},"PeriodicalIF":4.0,"publicationDate":"2025-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008803","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144929704","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}