Journal of Geophysical Research: Planets最新文献

{"title":"Estimating Primary Magmas From Mars With PRIMARSMELT: Implications for the Petrogenesis of Some Martian Rocks and the Thermal Evolution of Mars","authors":"Juan David Hernández-Montenegro,&nbsp;Paul D. Asimow,&nbsp;Claude T. Herzberg","doi":"10.1029/2024JE008508","DOIUrl":"https://doi.org/10.1029/2024JE008508","url":null,"abstract":"<p>Primary magmas form by partial melting in the mantle of a terrestrial planet and represent the starting material for building its crust. The compositions of primary magmas are critical for understanding the thermal history of planetary interiors, as they can be used to estimate mantle potential temperatures (<i>T</i>_<i>P</i>) and track changes in the conditions of mantle partial melting over time. Here, we introduce PRIMARSMELT, a new member of the PRIMELT software family, calibrated to estimate the composition of Martian primary magmas and their formation conditions. We applied PRIMARSMELT to a comprehensive database of basaltic compositions from Mars. Our results are consistent with their petrology, requiring olivine addition to restore fractionated compositions to their primary parents and olivine subtraction from cumulate rocks. Individual primary magma solutions provide insights into the petrogenesis of specific Martian meteorites, with implications for the near-primary nature of some primitive meteorites and the relationship between lithologies A and B in meteorite EETA 79001. Taken together, our results suggest nearly constant or potentially increasing mantle potential temperatures throughout the geological history of Mars. The average <i>T</i>_<i>P</i> for young shergottite meteorites is ∼1,442 ± 40°C, similar to ambient mantle temperatures inferred from geophysical models. In contrast, older basaltic rocks record potential temperatures as low as ∼1,320 ± 48°C for igneous clasts in meteorites NWA 7034/7533. We suggest that, rather than plume-related magmatism, shergottite meteorites record ambient mantle temperatures, with the thermal evolution trend possibly resulting from inefficient heat loss, as expected for a planet in stagnant-lid mode.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 11","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-11-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142588088","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":"Evidence for Magnetized Basin Ejecta on the Moon From Observations and Modeling of Demagnetized Craters","authors":"Hyeonhu Park,&nbsp;Ian Garrick-Bethell,&nbsp;Brandon C. Johnson,&nbsp;Ho Jin","doi":"10.1029/2024JE008420","DOIUrl":"https://doi.org/10.1029/2024JE008420","url":null,"abstract":"<p>The formation of lunar crustal magnetic anomalies is not well understood, and most anomalies are not associated with any obvious geologic features. To investigate further, we studied lunar craters from 100 to 400 km in diameter (totaling 305 craters) that may have demagnetized the crust. We find that the four craters Chaplygin, Keeler, Gauss, and Fermi are highly likely to have demagnetized the crust, based on our statistical methods. We modeled the magnetic source of these craters as a simple hole in a thin magnetized plate, representing the destruction of a surficial magnetized layer (Hypothesis 1). Alternatively, we also simulated the impact demagnetization of deeper-seated magnetism in the crust by shock and temperature (Hypothesis 2). Some interior magnetization remains unexplained under both hypotheses, but the destruction of a pre-existing surficial layer of magnetized material is consistent with the location of the peak in each crater's magnetic field. We also find three of the craters are inversely correlated with remotely sensed iron, further supporting our interpretation that the craters demagnetized a surficial layer. The four craters are located on magnetized ejecta deposits from the South Pole-Aitken, Orientale, and Crisium basins. Hence, these four craters further support the hypothesis that large provinces of magnetized material on the Moon arise from hot impact ejecta that cooled in a dynamo field.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 11","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-11-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008420","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142588158","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":"Massive Ice Sheet Basal Melting Triggered by Atmospheric Collapse on Mars, Leading to Formation of an Overtopped, Ice-Covered Argyre Basin Paleolake Fed by 1,000-km Rivers","authors":"P. B. Buhler","doi":"10.1029/2024JE008608","DOIUrl":"https://doi.org/10.1029/2024JE008608","url":null,"abstract":"<div>\u0000 \u0000 \u0000 <section>\u0000 \u0000 <p>Near the Noachian-Hesperian boundary (∼3.6 billion years ago), most of Mars' near-surface water inventory was likely frozen in large southern ice sheets and Mars' CO₂ atmosphere had eroded enough that it began to periodically collapse. Here, I report model results showing that thermal blanketing of a southern H₂O ice sheet by a CO₂ ice cap formed during atmospheric collapse would produce melt equivalent to ∼0.2–2.0 × Mars' present-day global near-surface H₂O inventory. I then model downstream flow, demonstrating the likely development of an ice-covered fluviolacustrine system with 1,000s-of-kilometer-long rivers, an overtopped Mediterranean-Sea-sized lake in Argyre Basin, and substantial water delivery into Margaritifer Terra and potentially Chryse Planitia. This study shows that a steady-state hydrologic cycle driven by pole-to-equator melt and equator-to-pole sublimation and atmospheric transport lasting 10⁵–10⁷ year could occur multiple times throughout a ∼10⁸-year window during which atmospheric pressure was low enough to collapse yet CO₂ and H₂O inventories and geothermal heat output were high enough to produce substantial meltwater. The nature of this proposed hydrologic cycle is consistent with estimates of the timing, duration, and intermittency of Noachian-Hesperian fluvial activity. Thus, meltwater release triggered by atmospheric collapse potentially played an important role in the intense pulse of Noachian-Hesperian fluvial activity: directly so for the Argyre-Margaritifer-Chryse system and perhaps indirectly for other catchments. Finally, this study demonstrates that large amounts of water can mobilize in a cold climate, driven by the same atmospheric collapse process occurring on Mars today, without invoking late-stage warming processes.</p>\u0000 </section>\u0000 </div>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 11","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008608","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142563026","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":"Infrared Spectroscopy of Lunar Core 73001: Upper Limit on Hydration in a Lunar Sample With No History of Exposure to Terrestrial Water Vapor","authors":"Paul G. Lucey,&nbsp;Ryan A. Zeigler,&nbsp;Lingzhi Sun,&nbsp;Abigail Flom,&nbsp;Andrea B. Mosie,&nbsp;Juliane Gross,&nbsp;Marley A. Chertok,&nbsp;Chiara Ferrari-Wong,&nbsp;Schelin M. Ireland,&nbsp;the ANGSA Team","doi":"10.1029/2024JE008389","DOIUrl":"https://doi.org/10.1029/2024JE008389","url":null,"abstract":"<p>The lunar surface exhibits an absorption band near 3 μm due to hydration, either water or hydroxyl. In most analyses, the band is variable at least in latitude and temperature. Hypotheses for the variability include infilling of the band by thermal emission, migration of molecular water along temperature gradients, and formation and destruction of metastable hydroxyl as solar wind hydrogen diffuses through lunar surface grains. The degree to which lunar soil exhibits an inherent hydration feature in the absence of environmental influences is an open question. The recent opening of Apollo core sample 73001 that was sealed in vacuum on the lunar surface and curated in dry nitrogen since its return from the Moon affords an opportunity to determine if lunar soil exhibits a spectral feature due to hydration isolated from the lunar environment. To that end, near the close of dissection of the core into samples for allocation to the lunar science community, we introduced an infrared spectrometer into the nitrogen purged curation cabinet and collected reflectance spectra of portions of the core between 2 and 4 μm. We found no evidence of absorption due to hydration to 1.1% band depth uncertainty. The measurements were relative to a diffuse aluminum standard, which itself could possibly absorb light at 3 μm due to a thin film of water; we estimate a possible negative bias of about 50 μg/g equivalent water absorption, leading to a final estimate of core water abundance of 50 μg/g ± 50 μg/g. This finding does not contradict prior estimates of lunar surface hydration as core sample 73001 is immature and may not have had sufficient opportunity to gather enough hydrogen from the solar wind or water from micrometeorites to form detectable hydration. After exposure of the core to laboratory atmosphere, a strong 3 μm absorption developed, equivalent to over 1,000 μg/g at a rate of about 5 μg/g per minute, illustrating the sensitivity of lunar materials to water contamination, and the effectiveness of curation of the sample.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 11","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008389","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142565993","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":"Multiple Impact Sources for Light Plains Around the Lunar South Pole","authors":"Barbara Giuri,&nbsp;Carolyn H. van der Bogert,&nbsp;Mark S. Robinson,&nbsp;Harald Hiesinger","doi":"10.1029/2024JE008605","DOIUrl":"https://doi.org/10.1029/2024JE008605","url":null,"abstract":"<p>We investigated the age and origin of 41 light plain deposits around the lunar south pole, using LRO data sets and successfully dated 22 of them using crater size-frequency distribution measurements. We find that deposits related to Schrödinger basin are ∼3.8 Ga old, including deposits on the Amundsen crater floor, which we interpret as Schrödinger basin ejecta. Six study areas date to ∼3.7 Ga, which reflect an additional large-scale or basin impact event post-Schrödinger - possibly Orientale. An additional two areas with younger isolated ages likely represent local impact sources. Finally, smooth, light plains-like, ejecta deposits around Shackleton crater were found to be Eratosthenian in age. Our findings show that light plain deposits originate from a combination of both basin and local ejecta materials. Thus, samples collected in the region will exhibit a diverse range of basin materials and ages representative of the ejecta from multiple impact events.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 11","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008605","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142565473","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":"Petrography, Crystallography, and Geochronology of Baddeleyite With Two Morphologies in a Chang'e-5 Lunar Basalt","authors":"Liying Huang,&nbsp;Yuchen Xu,&nbsp;Lang Qin,&nbsp;Yang Liu,&nbsp;Lixin Gu,&nbsp;Heng-Ci Tian,&nbsp;Jialong Hao,&nbsp;Feng Zhang,&nbsp;Wei Du,&nbsp;Jing Yang,&nbsp;Hejiu Hui,&nbsp;Wei Yang,&nbsp;Yangting Lin,&nbsp;Yongliao Zou","doi":"10.1029/2023JE007955","DOIUrl":"https://doi.org/10.1029/2023JE007955","url":null,"abstract":"<p>Baddeleyite (ZrO₂) is widespread in lunar basalts and frequently used for U-Pb geochronology of magmatic and impact events. The formation of baddeleyite involves two primary mechanisms: (a) crystallization from late-stage magma, and (b) decomposition of zircon under high-temperature (high-T) conditions. Baddeleyite with distinct formation mechanisms commonly displays different morphologies. In a Chang'e-5 lunar basalt, we report baddeleyite with two different morphologies, termed “singular type” and “aggregate type.” Petrographic and crystallographic analyses were conducted on both types of baddeleyite to understand their formation conditions and evolution processes. Despite the similarity in the morphology and mineral assemblages between the aggregate type baddeleyite and zircon decomposition products, the petrographic characteristics and the rarity of zircon in lunar basalts tend to suggest that both types of baddeleyite are derived from magma crystallization. Crystallographic relationships observed in both types indicate a phase transformation from the precursor tetragonal-ZrO₂/cubic-ZrO₂ or orthorhombic-ZrO₂ phase. Two potential scenarios are proposed for the formation of these microstructures: (a) direct crystallization of high symmetry ZrO₂ from magma, and (b) crystallization of baddeleyite from magma followed by a high-pressure (high-P) event causing its phase transition. However, due to unresolved scientific issues in both scenarios, an accurate evolutionary process cannot currently be determined. Therefore, extensive thermodynamic experiments are necessary to enhance our understanding of baddeleyite microstructures as indicators of P-T processes, providing insights into magmatism and the impact history of planetary bodies.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 11","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-10-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2023JE007955","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142563034","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":"Detailed Occurrence of Feather Features in Quartz in Experimentally Shocked Granite","authors":"Toshihiro Tada,&nbsp;Kosuke Kurosawa,&nbsp;Naotaka Tomioka,&nbsp;Takayoshi Nagaya,&nbsp;Junko Isa,&nbsp;Christopher Hamann,&nbsp;Haruka Ono,&nbsp;Takafumi Niihara,&nbsp;Takaya Okamoto,&nbsp;Takafumi Matsui","doi":"10.1029/2024JE008409","DOIUrl":"https://doi.org/10.1029/2024JE008409","url":null,"abstract":"<div>\u0000 \u0000 \u0000 <section>\u0000 \u0000 <p>Feather features (FFs) in quartz consist of a planar fracture (PF) and associated fine lamellae (FF lamellae; FFL) and have been observed in various natural impact structures. However, the mechanisms and conditions of FF formation are poorly understood. We conducted shock recovery experiments on granite using decaying compressive pulses to investigate the formation conditions of FFs. We characterized the recovered samples using an optical microscope equipped with a universal stage, a scanning electron microscope combined with an electron back-scattered diffraction detector, and a transmission electron microscope. We found that FFs are formed over a wide range of peak pressures (2–18 GPa) and that FFs can be divided into at least three types (I–III) based on the crystallographic orientation of the PFs and FFL, the angle between the orientation of the FFL and the propagation direction of the compression wave, and the presence/absence of amorphous silica in the FFL. The peak pressures that produce type I–III FFs are estimated to be &lt;12, 12–14, and &gt;16 GPa, respectively. We propose that FFs can be used as a shock barometer for quartz-bearing rocks.</p>\u0000 </section>\u0000 </div>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 11","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-10-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008409","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142555421","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":"Comprehensive Analysis of a Chloride-Rich Topographic Depression in Terra Sirenum, Mars: A Possible Lost Basin With Astrobiological Significance","authors":"Deepali Singh,&nbsp;Rishitosh K. Sinha,&nbsp;Kinsuk Acharyya","doi":"10.1029/2024JE008311","DOIUrl":"https://doi.org/10.1029/2024JE008311","url":null,"abstract":"<p>The hygroscopic nature of chlorides gives them the potential to provide a harbor for microbes to adapt and survive in extreme conditions, which is pertinent to Mars, given its evolution of climatic conditions. Moreover, observations of secondary hydrous minerals in chloride-rich regions have opened the case for a diverse geological environment on the Martian surface. Therefore, through comprehensive analysis, we aim to reconstruct the geological evolution of a chloride-rich basin within Terra Sirenum. We conducted morphological, morphometric, and mineralogical analyses of the basin and its surrounding area to determine its geological evolution, longevity, and environmental condi5tions during its activity. Subsequently, we carried out a discharge analysis of the surrounding valley networks and determined the water activity using ionic forms of the associated mineralogy. We observed bright-toned polygonal cracks within the basin as well as its surrounding terrain, suggesting that the basin extended beyond its present boundary. Mineralogical diversity and age dating of the basin and the surrounding area indicated different geochemical environments and cycles of wetting and drying until the late Hesperian. Whereas, sediment transport modeling suggests that the basin was hydrologically active for more than ten thousand years. Our results show a tell-tale signature of a large sedimentary basin and a large-scale geological process within the Terra Sirenum. The water activity modeling show that the geochemical composition of the basin was favorable to support the origin of life forms and/or sustain them and suggest promising aspects of the basin for future landing missions.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 11","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-10-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142555395","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":"Phase Transitions and Thermal Equation of State of Fe-9wt.%Si Applied to the Moon and Mercury","authors":"Meryem Berrada,&nbsp;Bin Chen,&nbsp;Keng-Hsien Chao,&nbsp;Juliana Peckenpaugh,&nbsp;Siheng Wang,&nbsp;Dongzhou Zhang,&nbsp;Phuong Nguyen,&nbsp;Jie Li","doi":"10.1029/2024JE008466","DOIUrl":"https://doi.org/10.1029/2024JE008466","url":null,"abstract":"<p>Accurate knowledge of the phase transitions and thermoelastic properties of candidate iron alloys, such as Fe-Si alloys, is essential for understanding the nature and dynamics of planetary cores. The phase diagrams of some Fe-Si alloys between 1 atm and 16 GPa have been back-extrapolated from higher pressures, but the resulting phase diagram of Fe_83.6Si_16.4 (9 wt.% Si) is inconsistent with temperature-induced changes in its electrical resistivity between 6 and 8 GPa. This study reports in situ synchrotron X-ray diffraction (XRD) measurements on pre-melted and powder Fe_83.6Si_16.4 samples from ambient conditions to 60 GPa and 900 K using an externally heated diamond-anvil cell. Upon compression at 300 K, the <i>bcc</i> phase persisted up to ∼38 GPa. The <i>hcp</i> phase appeared near 8 GPa in the pre-melted sample, and near 17 GPa in the powder sample. The appearance of the <i>hcp</i> phase in the pre-melted sample reconciles the reported changes in electrical resistivity of a similar sample, thus resolving the low-pressure region of the phase diagram. The resulting high-temperature Birch-Murnaghan equation of state (EoS) and thermal EoS based on the Mie-Gruneisen-Debye model of the <i>bcc</i> and <i>hcp</i> structures are consistent with, and complement the literature data at higher pressures. The calculated densities based on the thermal EoS of Fe-9wt.%Si indicate that both <i>bcc</i> and <i>hcp</i> phases agree with the reported core density estimates for the Moon and Mercury.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 11","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-10-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142555394","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":"Thermoluminescence and Apollo 17 ANGSA Lunar Samples: NASA's Fifty-Year Experiment and Prospecting for Cold Traps","authors":"Derek W. G. Sears,&nbsp;Alexander Sehlke,&nbsp;Harrison H. Schmitt,&nbsp;the ANGSA Science Team","doi":"10.1029/2024JE008358","DOIUrl":"https://doi.org/10.1029/2024JE008358","url":null,"abstract":"<div>\u0000 \u0000 \u0000 <section>\u0000 \u0000 <p>By placing Apollo 17 regolith samples in a freezer, and storing an equivalent set at room temperature, NASA effectively performed a 50-year experiment in the kinetics of natural thermoluminescence (TL) of the lunar regolith. We have performed a detailed analysis of the TL characteristics of four regolith samples: a sunlit sample near the landing site (70180), a sample 3 m deep near the landing site (70001), a sample partially shaded by a boulder (72320), and a sample completely shaded by a boulder (76240). We find evidence for a total of eight discrete TL peaks, five apparent in curves for samples in the natural state and seven in samples irradiated in the laboratory at room temperature. For each peak, we suggest values for peak temperatures and the kinetic parameters E (activation energy, i.e. “trap depth,” eV) and s (Arrhenius factor, s⁻¹). The lowest natural TL peak in the continuously shaded sample 76240 dropped in intensity by 60 ± 10% (1976 vs. present room temperature samples) and 43 ± 8% (freezer vs. room temperature samples) over the 50-year storage period, while sunlit and partially shaded samples (70001, 70180, 72321, 72320) showed no change. These results are consistent with the E and s parameters we determined. The large number of peaks, and the appearance of additional peaks after irradiation at room temperature, and literature data, suggest that glow curve peaks are present in lunar regolith at ∼100 K and their intensity can be used to determine temperature and storage time. Thus, a TL instrument on the Moon could be used to prospect for micro-cold traps capable of the storage of water and other volatiles.</p>\u0000 </section>\u0000 </div>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"129 10","pages":""},"PeriodicalIF":3.9,"publicationDate":"2024-10-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008358","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142525576","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}