Journal of Geophysical Research: Planets最新文献

{"title":"Anatomy of a Lunar Silicic Construct—The Wolf Crater Complex, Mare Nubium and Implications for Early Silicic Magmatism on the Moon","authors":"Himela Moitra,&nbsp;Sumit Pathak,&nbsp;Aditya K. Dagar,&nbsp;R. P. Rajasekhar,&nbsp;Satadru Bhattacharya,&nbsp;Moumita Akuria,&nbsp;Saibal Gupta","doi":"10.1029/2023JE008206","DOIUrl":"https://doi.org/10.1029/2023JE008206","url":null,"abstract":"<p>Silicic lithologies on planetary surfaces indicate magmatic evolutionary processes in their interiors. The Wolf crater complex within Mare Nubium on the Moon is one such silicic construct associated with a high thorium anomaly. This study integrates morphological, compositional, chronological and gravity anomaly analyses of high-resolution data from various lunar missions to establish this construct as a silicic volcanic caldera. Lobate flows with steeply sloping fronts indicate that the crater rims comprise high-viscosity silicic lavas, while the structurally controlled inner crater walls suggest caldera collapse triggered by magma depletion. In the crater rims, low Christiansen Feature position values reaffirm the presence of silicic lithologies, consistent with the low gravity anomaly signature beneath the complex, while spectroscopic data reveal low mafic mineral abundances and negligible hydration features. Chronological analyses yield silicic volcanism ages coeval with surrounding mare basalts (3.8–3.6 Ga), while intra-caldera basalts have 2.36–2.02 Ga ages, indicating prolonged magmatism in this region. Melting of suitable crustal protoliths like alkali gabbronorite/monzogabbro/troctolite by basaltic underplating is inferred to have generated silicic magmas that formed the Wolf volcanic complex, instead of basaltic magma fractionation or silicate-liquid immiscibility processes. Large impacts during the Late Heavy Bombardment may have enhanced partial melting of the mantle and created crustal fractures that facilitated the ascent of viscous silicic melts through the lunar crust. Contemporaneous existence of suitable protoliths and adequate crustal pathways for magma ascent may have controlled silicic volcanism on the Moon, and can explain the sporadic occurrence and overlapping ages of the lunar silicic constructs.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 9","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008206","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142244775","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":"Mapping and Characterizing the Northern Fan Deposits in Jezero Crater, Mars","authors":"Mohini J. Jodhpurkar,&nbsp;James F. Bell III,&nbsp;Sanjeev Gupta,&nbsp;Briony Horgan,&nbsp;Samantha Gwizd,&nbsp;Gwénaël Caravaca,&nbsp;Nicolas Randazzo","doi":"10.1029/2024JE008308","DOIUrl":"https://doi.org/10.1029/2024JE008308","url":null,"abstract":"<p>The northern inlet channel to Jezero crater (Sava Vallis) terminates in a fan-shaped depositional feature, part of which blends into the separate well-known western fan delta that is the field site for the Mars 2020 mission's <i>Perseverance</i> rover. Jezero's northern fan potentially represents either a second fan delta within the crater or a distal portion of the western fan. To constrain the fluvial and sedimentological history of Jezero and place the rover's in situ observations in proper geologic context, we photogeologically map the northern fan deposits at a larger mapping scale than previous studies, using ground-based imaging from the <i>Perseverance</i> rover for context. Fifteen map units are identified using HiRISE-based interpretations of geologic characteristics and inferred processes as well as crosscutting relative age relationships. Mapped units are also defined based on orbital data from CRISM and THEMIS to assess their compositional signatures. We interpret the northern fan deposits as older than the uppermost blocky unit in the western fan delta, suggesting that they were deposited contemporaneously with or prior to the deposition of the western fan, and under similar climate conditions. The eastern portion of the northern fan deposits shows evidence of fluvial deposition from Sava Vallis, while part of its western side could represent a distal part of the western fan delta. We synthesize our interpretations to present scenarios for the deposition of the northern and western fans, which can help constrain the history of both watersheds and place it into context within the broader Isidis basin region.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 9","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008308","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142230908","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":"Ferric Iron Evolution During Crystallization of the Earth and Mars","authors":"Laura Schaefer,&nbsp;Kaveh Pahlevan,&nbsp;Linda T. Elkins-Tanton","doi":"10.1029/2023JE008262","DOIUrl":"https://doi.org/10.1029/2023JE008262","url":null,"abstract":"<p>Magma ocean crystallization models that track <i>f</i>O₂ evolution can reproduce the D/H ratios of both the Earth and Mars without the need for exogenous processes. Fractional crystallization leads to compositional evolution of the bulk oxide components. Recent work suggests that metal-saturated magma oceans may contain near-present-day Fe³⁺ concentrations. We model the fractional crystallization of Earth and Mars, including Fe²⁺ and Fe³⁺ as separate components. We calculate Fe³⁺ partition coefficients for lower mantle minerals and compare the results of fractional crystallization for both Earth and Mars. We calculate oxygen fugacity (<i>f</i>O₂) at the surface as the systems evolve and compare them to constraints on the <i>f</i>O₂ of the last magma ocean atmosphere from D/H ratios, both with and without metal saturation. For Earth, we find that Fe³⁺ likely behaves incompatibly in the lower mantle in order to match the D/H constraint for whole mantle models, but shallow magma ocean models also provide reasonable matches. Disproportionation in whole mantle magma oceans likely overpredicts the amount of Fe³⁺ and metal that form or require subsequent reduction to return to present-day values. For Mars, we cannot match the D/H constraints on last <i>f</i>O₂ unless the magma ocean begins with &lt;50% of the predicted Fe³⁺, but better match the present day mantle redox. We show that Fe³⁺ partitioning has a measurable effect on magma ocean redox, and that it evolves throughout the magma ocean's lifetime. We highlight the need for additional experimental constraints on ferric iron mineral/melt partitioning and more thermodynamic data for the Fe-disproportionation reaction.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 9","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142230907","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":"Analysis of the Cessation of Convection in Mercury's Mantle","authors":"C. Jain,&nbsp;V. S. Solomatov","doi":"10.1029/2024JE008365","DOIUrl":"https://doi.org/10.1029/2024JE008365","url":null,"abstract":"<p>The question of whether the present-day mantle of Mercury is undergoing convection remains unresolved. We address this issue by estimating the minimum value of the core-mantle boundary (CMB) temperature needed to support mantle convection and considering the time required to cool the mantle below this threshold. A simple mathematical analysis of the cooling of the core, based on the assumption of a quasi-steady-state thermal equilibrium of Mercury's mantle, shows that the CMB temperature falls to the critical temperature for cessation of convection roughly halfway through the planet's evolutionary history. To first order, the duration of subsolidus convection does not depend on the absolute value of the viscosity. It depends primarily on parameters that control the viscosity function, such as the stress exponent and the activation energy. Our results based on conventional assumptions suggest the absence of present-day mantle convection in Mercury, which is consistent with numerical models of Mercury's thermal history. However, because of large uncertainties in the controlling parameters, the possibility of still ongoing mantle convection on Mercury cannot be ruled out.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 9","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142160218","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":"Deterministic Model for Asteroid Thermal Evolution With Fragmentation and Reassembly Into a Gravitational Aggregate","authors":"J. Ren,&nbsp;M. A. Hesse,&nbsp;N. Dygert,&nbsp;M. P. Lucas","doi":"10.1029/2023JE007898","DOIUrl":"https://doi.org/10.1029/2023JE007898","url":null,"abstract":"<p>We present a model for the thermal evolution of asteroids that experience catastrophic fragmentation and reassembly into a gravitational aggregate. The three stage model comprises the initial radiogenic heating, fragmentation and cooling, and reassembly into a porous gravitational aggregate. The heat loss during catastrophic fragmentation is largely determined by the production of small particles that equilibrate thermally with ambient space. To determine this heat loss we combine a power-law for the cumulative fragment mass distribution with analytic solutions for conductive cooling. To keep the model deterministic we fragment the parent body and reassemble the gravitational aggregate in shells ordered in decreasing volume. We use the resulting model to show that catastrophic fragmentation can lead to significant heat loss despite the short reassembly times (e.g., <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≤</mo>\u0000 </mrow>\u0000 <annotation> ${le} $</annotation>\u0000 </semantics></math>1 year), due to the production of many small fragments. Despite the heat loss during fragmentation, the reassembled gravitational aggregate will retain more heat than the undisturbed parent body in the long term, due to the formation of an insulating megaregolith. Applied to the H-chondrite parent body, our model can reproduce both the fast cooling rates at high temperatures and slow cooling rates at low temperature.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 9","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142152187","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":"Consus Crater on Ceres: Ammonium-Enriched Brines in Exchange With Phyllosilicates?","authors":"A. Nathues,&nbsp;M. Hoffmann,&nbsp;R. Sarkar,&nbsp;P. Singh,&nbsp;J. Hernandez,&nbsp;J. H. Pasckert,&nbsp;N. Schmedemann,&nbsp;G. Thangjam,&nbsp;E. Cloutis,&nbsp;K. Mengel,&nbsp;M. Coutelier","doi":"10.1029/2023JE008150","DOIUrl":"https://doi.org/10.1029/2023JE008150","url":null,"abstract":"<p>Ceres is a partially differentiated dwarf planet located in the main asteroid belt. Consus crater (diameter ∼64 km) is one of the oldest impact features (∼450 Ma) on the Cerean surface that surprisingly still shows a large variety of color lithologies, including exposures of bright material, which are thought to be brine residues. Here, we present new results that help in understanding the structure and composition of the Cerean crust. These results were deduced by using newly processed Dawn Framing Camera (FC) color imagery and FC clear filter images combined with infrared spectral data of Dawn's Visible and Infrared Spectrometer (VIR). Consus exhibits a variety of color lithologies, which we describe in detail. Interestingly, we found three spectrally different types of bright material exposed by a large old crater on Consus' floor. One of these, the yellowish bright material (Nathues et al., 2023, https://www.hou.usra.edu/meetings/lpsc2023/pdf/1073.pdf) and its modification, shows spectral signatures consistent with ammonium-enriched smectites. We hypothesize that the ammonium in these smectites stems from contact with ascending brines, originating from a low-lying former brine ocean that has been enriched in ammonium during the differentiation and freezing process of the Cerean crust. This enrichment is mainly due to ammonium uptake by sheet silicates. If such an ammonium enrichment occurred over long-time scales on a global scale, this process may explain the vast presence of ammonium on the Cerean surface. Therefore, an outer solar system origin of Ceres is possibly not needed to explain the global presence of ammonium.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 9","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008150","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142152298","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":"Shadowgraph Measurements of Rotating Convective Planetary Core-Style Flows","authors":"Jewel A. Abbate,&nbsp;Jonathan M. Aurnou","doi":"10.1029/2024JE008471","DOIUrl":"https://doi.org/10.1029/2024JE008471","url":null,"abstract":"<p>The local scale of rotating convection, <i>ℓ</i>, is a fundamental parameter in many turbulent geophysical and astrophysical fluid systems, yet it is often poorly constrained. Here we conduct rotating convection laboratory experiments analogous to convecting flows in planetary cores and subsurface oceans to obtain measurements of the local scales of motion. Utilizing silicone oil as the working fluid, we employ shadowgraph imagery to visualize the flow, from which we extract values of the characteristic cross-axial scale of convective columns and plumes. These measurements are compared to the theoretical values of the critical onset length scale, <i>ℓ</i>_<i>crit</i>, and the turbulent length scale, <i>ℓ</i>_<i>turb</i>. Our experimentally obtained length scale measurements simultaneously agree with both the onset and turbulent scale predictions across three orders of magnitude in convective supercriticality <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>(</mo>\u0000 <mrow>\u0000 <mn>1</mn>\u0000 <msup>\u0000 <mn>0</mn>\u0000 <mn>2</mn>\u0000 </msup>\u0000 <mo>≲</mo>\u0000 <mover>\u0000 <mrow>\u0000 <mi>R</mi>\u0000 <mi>a</mi>\u0000 </mrow>\u0000 <mo>∼</mo>\u0000 </mover>\u0000 <mo>≲</mo>\u0000 <mn>1</mn>\u0000 <msup>\u0000 <mn>0</mn>\u0000 <mn>5</mn>\u0000 </msup>\u0000 </mrow>\u0000 <mo>)</mo>\u0000 </mrow>\u0000 <annotation> $(1{0}^{2}lesssim tilde{Ra}lesssim 1{0}^{5})$</annotation>\u0000 </semantics></math>, a correlation that is consistent with inferences made in prior studies. We further explore the nature of this correlation and its implications for geophysical and astrophysical systems.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 9","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008471","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142137858","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":"Relationships Between HCl, H2O, Aerosols, and Temperature in the Martian Atmosphere: 1. Climatological Outlook","authors":"K. S. Olsen,&nbsp;A. A. Fedorova,&nbsp;D. M. Kass,&nbsp;A. Kleinböhl,&nbsp;A. Trokhimovskiy,&nbsp;O. I. Korablev,&nbsp;F. Montmessin,&nbsp;F. Lefèvre,&nbsp;L. Baggio,&nbsp;J. Alday,&nbsp;D. A. Belyaev,&nbsp;J. A. Holmes,&nbsp;J. P. Mason,&nbsp;P. M. Streeter,&nbsp;K. Rajendran,&nbsp;M. R. Patel,&nbsp;A. Patrakeev,&nbsp;A. Shakun","doi":"10.1029/2024JE008350","DOIUrl":"https://doi.org/10.1029/2024JE008350","url":null,"abstract":"<p>Detecting trace gases such as hydrogen chloride (HCl) in Mars' atmosphere is among the primary objectives of the ExoMars Trace Gas Orbiter (TGO) mission. Terrestrially, HCl is closely associated with active volcanic activity, so its detection on Mars was expected to point to some form of active magmatism/outgassing. However, after its discovery using the mid-infrared channel of the TGO Atmospheric Chemistry Suite (ACS MIR), a clear seasonality was observed, beginning with a sudden increase in HCl abundance from below detection limits to 1–3 ppbv in both hemispheres coincident with the start of dust activity, followed by very sudden and rapid loss at the southern autumnal equinox. In this study, we have investigated the relationship between HCl and atmospheric dust by making comparisons in the vertical distribution of gases measured with ACS and aerosols measured co-located with the Mars Climate Sounder (MCS). This study includes HCl, water vapor, and ozone measured using ACS MIR, water vapor and temperature measured with the near infrared channel of ACS, and temperature, dust opacity, and water ice opacity measured with MCS. In part 1, we show that dust loading has a strong impact in temperature, which controls the abundance of water ice and water vapor, and that HCl is very closely linked to water activity. In part 2, we investigate the quantitative correlations between each quantity and discuss the possible source and sinks of HCl, their likelihood given the correlations, and any issues arising from them.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 8","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-08-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008350","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142077815","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":"Relationships Between HCl, H2O, Aerosols, and Temperature in the Martian Atmosphere: 2. Quantitative Correlations","authors":"K. S. Olsen,&nbsp;A. A. Fedorova,&nbsp;D. M. Kass,&nbsp;A. Kleinböhl,&nbsp;A. Trokhimovskiy,&nbsp;O. I. Korablev,&nbsp;F. Montmessin,&nbsp;F. Lefèvre,&nbsp;L. Baggio,&nbsp;J. Alday,&nbsp;D. A. Belyaev,&nbsp;J. A. Holmes,&nbsp;J. P. Mason,&nbsp;P. M. Streeter,&nbsp;K. Rajendran,&nbsp;M. R. Patel,&nbsp;A. Patrakeev,&nbsp;A. Shakun","doi":"10.1029/2024JE008351","DOIUrl":"https://doi.org/10.1029/2024JE008351","url":null,"abstract":"<p>The detection of hydrogen chloride (HCl) in the atmosphere of Mars was among the primary objectives of the ExoMars Trace Gas Orbiter (TGO) mission. Its discovery using the Atmospheric Chemistry Suite mid-infrared channel (ACS MIR) showed a distinct seasonality and possible link to dust activity. This paper is part 2 of a study investigating the link between HCl and aerosols by comparing gas measurements made with TGO to dust and water ice opacities measured with the Mars Climate Sounder (MCS). In part 1, we showed, and compared, the seasonal evolution of vertical profiles of HCl, water vapor, temperature, dust opacity, and water ice opacity over the dusty periods around perihelion (solar longitudes 180°–360°) across Mars years 34–36. In part 2, we investigated the quantitative correlations in the vertical distribution between each quantity, as well as ozone. We show that there is a strong positive correlation between HCl and water vapor, which is expected due to fast photochemical production rates for HCl when reacting with water vapor photolysis products. We also show a strong positive correlation between water vapor and temperature, but are unable to show any correlation between temperature and HCl. There are weak correlations between the opacities of dust and water ice, and dust and water vapor, but only very low correlations between dust and HCl. We close with a discussion of possible sources and sinks and that interactions between HCl and water ice are the most likely for both, given the inter-comparison.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 8","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-08-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008351","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142077920","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":"Integrated Spectral and Compositional Analysis for the Lunar Tsiolkovskiy Crater","authors":"Gloria Tognon,&nbsp;Francesca Zambon,&nbsp;Cristian Carli,&nbsp;Matteo Massironi,&nbsp;Lorenza Giacomini,&nbsp;Riccardo Pozzobon,&nbsp;Giulia Salari,&nbsp;Federico Tosi,&nbsp;Jean-Philippe Combe,&nbsp;Sergio Fonte","doi":"10.1029/2023JE008272","DOIUrl":"https://doi.org/10.1029/2023JE008272","url":null,"abstract":"<p>Remote sensing observations represent the primary means in the production of geologic maps of planetary surfaces. However, they do not provide the same level of detail as Earth's geologic maps, which rely also on field observations and laboratory analyses. Color-derived basemaps can help to bridge this gap by highlighting peculiar surface and compositional properties. Here, we analyzed the spectral properties of the lunar Tsiolkovskiy crater through the definition of spectral units summarizing the information enclosed by a set of selected spectral parameters. We then performed a compositional analysis of the newly derived spectral units that helped us in discriminating the presence and relative abundance of the main mineralogical phases on the Moon. As a final step, we produced a geo-stratigraphic map of the Tsiolkovskiy crater integrating in a single mapping product both morphologic, stratigraphic and compositional information. The basaltic infilling of the crater is distinguished by three spectral units associated with distinct effusive events presenting a different composition. On the central peak, plagioclase and olivine suggest the presence of Mg-suite rocks from the lower crust. The continuous ejecta deposits are mostly characterized by impact melts and shocked materials rich in glass or agglutinates related to more mature terrains from which occasionally appear fresher anorthositic and gabbroic outcrops exposed by the inward sliding of the crater walls. Overall, the geo-stratigraphic map allows inferring compositional variations associated with the different morpho-stratigraphic units, which clarify and elaborate on the compositional heterogeneities within the lunar crust and the Tsiolkovskiy crater, and its geologic evolutionary history.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 8","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-08-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008272","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142045287","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}