Journal of Geophysical Research: Planets最新文献

{"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}

{"title":"Insight Into Venusian Ridge Belts With Maps, Models, and Earth Analogs","authors":"K. T. Crane,&nbsp;P. K. Byrne","doi":"10.1029/2024JE008625","DOIUrl":"https://doi.org/10.1029/2024JE008625","url":null,"abstract":"<p>Ridge belts are globally distributed mountain belts on Venus comprised of closely spaced shortening structures superimposed on longer wavelengths (1 km spacing over 30–400 km-wide belt), positive topography often surrounded by topographically smooth, intact crustal blocks. Although interpreted as large-scale shortening systems, we understand little about the causes of that shortening. On Earth, analogous mountain belts represent a range of crustal or tectonic block boundary collisions, and so the concentration of ridge belt structures could likewise be linked to crustal block collision at a reactivated suture or pre-existing crustal weakness. We can examine this hypothesis using structural maps, cross sections, and three-dimensional models of faults associated with ridge belts. We produced three detailed structural maps and 11 cross sections, which show that the ridge belts we selected represent two shortening styles-one with a single dominant fault, and one with two oppositely verging faults. These results may indicate that fresh or reactivated block collisions lead to ridge belt development.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143646139","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":"Global Transport of Chlorine Species in the Martian Atmosphere and the Resulting Surface Distribution of Perchlorates","authors":"K. Rajendran,&nbsp;P. M. Streeter,&nbsp;S. R. Lewis,&nbsp;M. K. D. Duffy,&nbsp;J. A. Holmes,&nbsp;K. S. Olsen,&nbsp;O. Korablev,&nbsp;M. R. Patel","doi":"10.1029/2024JE008537","DOIUrl":"https://doi.org/10.1029/2024JE008537","url":null,"abstract":"&lt;p&gt;Recent observations by instruments aboard the ExoMars Trace Gas Orbiter (TGO) have revealed the seasonal presence of hydrogen chloride (&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mtext&gt;HCl&lt;/mtext&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; $text{HCl}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;) in the Martian atmosphere. This discovery may have important implications for Martian photochemistry as chlorine species are chemically active, and it may provide a link between the atmosphere and known surface reservoirs of chlorine. However, the global distribution of atmospheric &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mtext&gt;HCl&lt;/mtext&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; $text{HCl}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; is unknown beyond the very sparse TGO observations, and the source and sink processes driving the observed variability of &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mtext&gt;HCl&lt;/mtext&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; $text{HCl}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; are not currently understood. We used a Martian global climate model to investigate, for the first time, the spatial distribution of chlorine species in the Martian atmosphere, and the resulting distribution of surface perchlorates formed via adsorption of atmospheric chlorine species. We adapted an existing Martian photochemical scheme to include gas-phase chlorine chemistry with HCl as the source species, and the resulting atmospheric perchloric acid was allowed to deposit onto the Martian surface via a heterogeneous adsorption scheme. We found that odd-oxygen (&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;O&lt;/mi&gt;\u0000 &lt;mo&gt;,&lt;/mo&gt;\u0000 &lt;msub&gt;\u0000 &lt;mi&gt;O&lt;/mi&gt;\u0000 &lt;mn&gt;3&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; $mathrm{O},{mathrm{O}}_{3}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;) and odd-hydrogen (&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;H&lt;/mi&gt;\u0000 &lt;mo&gt;,&lt;/mo&gt;\u0000 &lt;mtext&gt;OH&lt;/mtext&gt;\u0000 &lt;mo&gt;,&lt;/mo&gt;\u0000 &lt;msub&gt;\u0000 &lt;mtext&gt;HO&lt;/mtext&gt;\u0000 &lt;mn&gt;2&lt;/mn&gt;\u0000 &lt;/msub&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt; $mathrm{H},text{OH},{text{HO}}_{2}$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;) species play a major role in controlling the distribution of atmospheric chorine species. Surface perchlorate deposition was found to occur preferentially at high latitudes; in the tropics, the perchlorate distribution was anti-correlated with surface thermal inertia and agreed qualitatively with ob","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008537","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143639004","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":"Late-Stage Aqueous Activity at Gale Crater, Mars, Recorded by Sediment Fans Eroded From Aeolis Mons","authors":"Joel M. Davis,&nbsp;Sanjeev Gupta,&nbsp;Peter M. Grindrod,&nbsp;Steven G. Banham,&nbsp;Amanda Rudolph,&nbsp;Sharon A. Wilson,&nbsp;John A. Grant,&nbsp;Rebecca M. E. Williams,&nbsp;Edwin S. Kite,&nbsp;Amelie L. Roberts,&nbsp;Emma Harris,&nbsp;Gerhard Paar","doi":"10.1029/2024JE008808","DOIUrl":"https://doi.org/10.1029/2024JE008808","url":null,"abstract":"<p>Gale crater, the landing site of NASA's <i>Curiosity</i> rover, and the mountain at its center, Aeolis Mons, hosts an extensive record of sedimentary rocks, which provide a window into the climate history of Mars. <i>Curiosity</i> has demonstrated that Gale hosted long-lived lakes early in its history, indicating warm, quiescent surface conditions, before transitioning into a period of heightened aridity. Recent investigations using orbital data have suggested that the surface of Mars was intermittently wet late in its history. However, an ongoing challenge is linking these orbital observations to on-ground investigations by rovers. Here we use combined orbital image and topographic data sets to investigate a series of sediment fans and related catchment regions within the wider Gale crater, and regional to <i>Curiosity</i>'s exploration zone. These systems can be stratigraphically linked to the sedimentary rocks that <i>Curiosity</i> has investigated. We find that most of the sediment fans are likely alluvial fans, recording intermittent flow conditions, with deposition concentrated near the base of Aeolis Mons. The sediment fans are intermixed with landslide deposits and source canyons have been significantly backfilled. We find that these systems formed after regional geological units which <i>Curiosity</i> has shown to record periods of prolonged aridity. Our study demonstrates that intermittent surface water was likely to be present regionally with Gale crater during or after the exhumation of Aeolis Mons. <i>Curiosity</i> may be able to constrain the source and duration of these late-stage flow events as it ascends Aeolis Mons.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008808","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143646071","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":"Hydroxylation and Hydrogen Diffusion in Lunar Samples: Spectral Measurements During Proton Irradiation","authors":"Li Hsia Yeo,&nbsp;Anastasis Georgiou,&nbsp;Liam Morrissey,&nbsp;William Farrell,&nbsp;Jason McLain","doi":"10.1029/2024JE008334","DOIUrl":"https://doi.org/10.1029/2024JE008334","url":null,"abstract":"<p>Widespread OH/<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>H</mi>\u0000 <mn>2</mn>\u0000 </msub>\u0000 </mrow>\u0000 <annotation> ${mathrm{H}}_{2}$</annotation>\u0000 </semantics></math>O has been detected across the lunar surface, but its origin remains a matter of active investigation. We present laboratory measurements of Apollo-17 samples LS 78421 and LS 73131 that demonstrate, in situ, the formation of OH/<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>H</mi>\u0000 <mn>2</mn>\u0000 </msub>\u0000 </mrow>\u0000 <annotation> ${mathrm{H}}_{2}$</annotation>\u0000 </semantics></math>O during irradiation by energetic hydrogen ions similar to the solar wind. Results unambiguously show the growth of the <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 </mrow>\u0000 <annotation> ${sim} $</annotation>\u0000 </semantics></math>3 <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>μ</mi>\u0000 </mrow>\u0000 <annotation> ${upmu }$</annotation>\u0000 </semantics></math>m spectral band due to hydrogen irradiation alone with no contribution from terrestrially adsorbed water. Significant variations in the <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 </mrow>\u0000 <annotation> ${sim} $</annotation>\u0000 </semantics></math>3 <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>μ</mi>\u0000 </mrow>\u0000 <annotation> ${upmu }$</annotation>\u0000 </semantics></math>m band characteristics and position are measured between LS 78421, LS 73131, and a control of crushed silica, reflecting the unique crystal structures and chemical environments within each sample. By cycling sample temperatures to 400 K (lunar dayside maximum), we highlight the role of hydrogen diffusion in the dynamics of OH/<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msub>\u0000 <mi>H</mi>\u0000 <mn>2</mn>\u0000 </msub>\u0000 </mrow>\u0000 <annotation> ${mathrm{H}}_{2}$</annotation>\u0000 </semantics></math>O within the lunar soil. Diffusion activation energies of 0.66–0.75 eV and 0.72–0.81 eV are obtained for LS 78421 and LS 73131, respectively.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008334","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143632690","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":"Statistical Distribution of Chorus Waves in Jupiter's Magnetosphere Based on Galileo and Juno Observations","authors":"Peng Lu,&nbsp;Xing Cao,&nbsp;Binbin Ni,&nbsp;Shaobei Wang,&nbsp;Minyi Long","doi":"10.1029/2024JE008818","DOIUrl":"https://doi.org/10.1029/2024JE008818","url":null,"abstract":"<p>Whistler mode chorus waves are commonly observed in planetary magnetospheres and play an important role in the acceleration and loss of planetary energetic electrons. By combining the observations from Juno (PJ01 to PJ56) and Galileo, we conduct a detailed statistical analysis of the spatial distribution of the occurrence rates and averaged amplitudes of chorus waves in the Jovian magnetosphere. The statistical results show that chorus waves are widely distributed at 5 &lt; M-shell &lt; 15 within the magnetic latitudes (MLats) of &lt; 50°, with the averaged amplitudes ranging from 3 to ∼50 pT. The most intense waves are found in the duskside inner magnetosphere at 8 &lt; M-shell &lt; 11 near the equatorial region (MLat &lt; 20°). The wave amplitudes decrease significantly with increasing MLat, and are an order of magnitude larger on the duskside compared to the dawnside. Based on the statistical results, we develop an empirical model of the distribution of chorus wave amplitudes as a function of M-shell, magnetic local time and MLat, which can provide key information of the waves for future studies of resonant wave-particle interactions between chorus waves and energetic electrons at Jupiter.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143622523","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":"Fluvial Reworking Eliminates Small Craters, But Does Not Meaningfully Bias the Mars Interbedded-Crater Record","authors":"Andrew J. Moodie,&nbsp;Timothy A. Goudge","doi":"10.1029/2023JE008183","DOIUrl":"https://doi.org/10.1029/2023JE008183","url":null,"abstract":"<p>Interpreting the structures, morphology, and chemistry of the exposed stratigraphic record on Mars is complicated by ancient surface processes that have variably removed parts of the record. Previous research has used the lack of smaller craters (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≤</mo>\u0000 </mrow>\u0000 <annotation> ${le} $</annotation>\u0000 </semantics></math>50 m diameter) interbedded with fluvial deposits to constrain atmospheric pressure when rivers were active on Mars; the notion being that higher atmospheric pressure would have prevented smaller craters from forming. We hypothesize that contemporaneous channel lateral migration and avulsion could have reworked sedimentary deposits and eliminated craters from the stratigraphic record, thereby undermining atmospheric paleo-pressure interpretations. To test this hypothesis, we simulated coeval river-delta development and crater production, and quantified crater preservation in resulting stratigraphy. We document widespread crater rim degradation (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 </mrow>\u0000 <annotation> ${sim} $</annotation>\u0000 </semantics></math>67% of craters <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≤</mo>\u0000 </mrow>\u0000 <annotation> ${le} $</annotation>\u0000 </semantics></math>50 m at least partially eroded), and observe a marked increase in preservation with increasing crater diameter. That is to say, fluvial reworking preferentially removes smaller craters from the stratigraphic record. However, synthetic crater-diameter distributions incorporating fluvial reworking effects do not reproduce observations on Mars, because many smaller craters generated remain preserved in the simulated stratigraphy. We find that, although river channels are sometimes in the right place to eliminate crater deposits from the stratigraphic record, production of smaller craters outpaces fluvial reworking under all modeled circumstances, and that a higher pressure ancient atmosphere is necessary to reproduce observations (i.e., consistent with existing interpretations of interbedded crater records). Our findings therefore bolster studies that assert fluvial reworking is not a primary control on smaller interbedded crater counts on Mars.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE008183","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143602465","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 Local Dust Storms Associated With Extratropical Cyclones in Arcadia Planitia","authors":"K. Ogohara","doi":"10.1029/2024JE008455","DOIUrl":"https://doi.org/10.1029/2024JE008455","url":null,"abstract":"<p>Dust storm events in western Arcadia Planitia were extracted from visible images obtained by the Mars Orbiter Camera onboard the Mars Global Surveyor (MGS) spacecraft using deep learning. Local dust storms in this region were concentrated between roughly the northern autumn and spring equinoxes, except around the northern winter solstice. In addition, transient eddies (traveling weather systems) with wavenumber 3 in the lower atmosphere tended to be amplified when the local dust storms were frequent. The atmospheric environment around this area when the dust storms were observed was investigated via a composite analysis of the Mars reanalysis data set, and it was found that local dust storms tended to be observed near the southern edge of a warm and southerly wind anomaly associated with a transient eddy with wavenumber 3. Because the MGS observations are limited to around 14:00 local time, there is a 1-Martian-day uncertainty in the timing of dust storm onsets. Using backward trajectory analysis, we estimated the location and time of each dust storm onset in the 24 Martian hours prior to the time when the dust storm was observed. The results still show that the observed dust storms tend to occur in and around the warm and southerly wind anomalies. This warm inflow from the south into the extratropical cyclone made the lower atmosphere less stable convectively during the day and enhanced the southerly wind on the northern slope of Elysium Mons during the night to induce the formation of the meso-scale dust storms.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143622379","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":"Solidification and Differentiation of a Mushy Lunar Magma Ocean: 3D Numerical Modeling","authors":"Yizhuo Zhang,&nbsp;Nan Zhang,&nbsp;Meng Tian,&nbsp;Yun Liu","doi":"10.1029/2024JE008532","DOIUrl":"https://doi.org/10.1029/2024JE008532","url":null,"abstract":"<p>The lunar magma ocean (LMO) was formerly proposed to explain the anorthositic nature of the lunar crust as constrained by returned samples. The LMO was conventionally thought to experience a sequence of fractional crystallization, with the crust formed through plagioclase floatation. Such a conventional thinking, however, suffers from being unable to account for the <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 </mrow>\u0000 <annotation> ${sim} $</annotation>\u0000 </semantics></math>200 Myr lunar crustal formation timescale and from contradicting the measured overlapping ages between the lunar Mg-suite and ferroan anorthosites. Coming to the rescue is the slushy/mushy lunar magma ocean scenario that can sustain lunar crustal magmatism over <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 </mrow>\u0000 <annotation> ${sim} $</annotation>\u0000 </semantics></math>200 Myr. In this study, we develop a 3D spherical numerical model to quantify the solidification and differentiation of the Moon over its history. The model includes thermal and compositional mantle convection, a parameterized phase diagram for melting involving the two components of anorthite and olivine (representative of fertile and refractory components, respectively), porous melt segregation, and parameterized melt extraction via near-surface dikes. We find that the thermal effect of melt migration is so strong that it leads to a negative correlation between the duration of the crustal magmatism and the reference permeability of the mushy interior. Our results also affirm the previous scaling analysis that points out the possibility of <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 </mrow>\u0000 <annotation> ${sim} $</annotation>\u0000 </semantics></math>200-Myr lunar crustal growth from the slushy mantle. By considering compositional buoyancy, our model also identifies a possible overturn mechanism during the Moon's mushy stage, potentially reconciling the magma ocean theory with the observed age overlapping between the lunar Mg-suite and ferroan anorthosites.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143595623","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":"Composition, Mineralogy, and Noble Gas Content of Apollo 17 Particles and Soils From the 73002 Drive Tube","authors":"Barbara A. Cohen,&nbsp;Natalie M. Curran,&nbsp;Sarah N. Valencia,&nbsp;Catherine M. Corrigan,&nbsp;Emma S. Bullock,&nbsp;Elana G. Alevy,&nbsp;Scott A. Eckley,&nbsp;the ANGSA Science Team","doi":"10.1029/2024JE008329","DOIUrl":"https://doi.org/10.1029/2024JE008329","url":null,"abstract":"<p>As part of the Apollo Next-Generation Sample Analysis (ANGSA) program, we provide bulk composition, mineralogy, petrology, and noble gas assays of lunar particles and soils from the top half of the 73001/2 double-drive tube (i.e., 73002) studied by the ANGSA consortium. The particles are derived from lithologies of the South Massif, including anorthosites, anorthositic breccias, high-Ti basalts, noritic impact-melt breccias, agglutinates, and regolith breccias. The impact-melt breccias are distinguished by their inclusion of high-Mg spinel that may extend the compositional family of pink spinel troctolites. The noble gas data provide cosmic-ray exposure ages representing the emplacement of the light mantle unit at 60 Ma preceded by soil exposure in an avalanche-emplaced surface around 100 Ma. These measurements provide additional insight into the geologic evolution of the Apollo 17 site and the light mantle unit sampled by the double-drive tube.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 3","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-03-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008329","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143595617","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}