Journal of Geophysical Research: Planets最新文献

{"title":"Differences in Rock Magnetic Properties From Heterogeneous Weathering of the LL7 Chondrite Northwest Africa 12780","authors":"Haijun Li,&nbsp;Huapei Wang","doi":"10.1029/2024JE008768","DOIUrl":"https://doi.org/10.1029/2024JE008768","url":null,"abstract":"<p>Meteorites preserve valuable remanent magnetization from the early solar system. However, the residence on the Earth's surface often leads to the formation of iron oxides, which can alter or obliterate the primary remanence and complicate the paleomagnetic data interpretation. The weathering degree varies significantly depending on residence time, location, climate, and the chemical composition of the meteorite. Additionally, individual meteorites can exhibit varying oxidation degrees within a single stone due to partial burial in soil. This study examines the LL7 chondrite Northwest Africa 12780, revealing heterogeneous weathering across different parts of the meteorite. While one part shows extensive metal oxidation, another remains unoxidized. Although most oxidized subsamples contain paramagnetic iron oxides, maghemite is observed in some oxidized subsamples. Our findings highlight the presence of heterogeneous weathering in meteorites, which leads to the formation of various iron oxides, including maghemite, potentially acquiring chemical remanent magnetization and overprinting primary remanence. This also indicates that certain subsamples may retain their primary remanence even in weathered meteorites. However, systematic investigations are necessary to eliminate the influence of ferromagnetic iron oxides.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 5","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143939527","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":"Micro X-Ray Diffraction Observations and Calibration of Experimentally Shocked Plagioclase Feldspars: Comparison With Raman Spectroscopic Observations","authors":"Fengke Cao,&nbsp;Roberta L. Flemming,&nbsp;Matthew R. M. Izawa,&nbsp;Steven J. Jaret,&nbsp;Jeffrey R. Johnson","doi":"10.1029/2024JE008574","DOIUrl":"https://doi.org/10.1029/2024JE008574","url":null,"abstract":"<p>Plagioclase feldspar is a ubiquitous mineral found in planetary bodies such as Earth, Moon, Mars, large igneous asteroids such as Vesta, numerous achondrites, and every class of chondritic meteorite. Because all solid planetary bodies are potentially subject to hypervelocity impacts, understanding the shock response of plagioclase enables a better understanding of the geological histories of planetary bodies. This study investigates the response of andesine and bytownite to high-pressure shock waves using micro-XRD and Raman. Fourteen andesine and 11 bytownite samples, which had been previously shocked to peak pressures of 0–56 GPa, were examined. Micro-XRD revealed characteristic signatures of shock damage, including weakened diffraction intensities and heightened background signal, reflecting structural collapse under high pressures. Andesine-bearing rock showed the onset of amorphization at 28.4–29.6 GPa, progressing to complete amorphization at 47.5–50 GPa. Bytownite-bearing rock displayed a similar trend but with higher pressure thresholds: partial amorphization occurred at 25.5–27.0 GPa, and complete amorphization at 38.2–49 GPa. To quantify the degree of shock experienced by plagioclase minerals, we measured the Full Width at Half Maximum (FWHMχ) of Debye rings (from 2D XRD images) for samples across different shock levels. We established linear regression models between ΣFWHMχ and peak shock pressure for both andesine (0–28.4 GPa) and bytownite (0–25.5 GPa) using data from samples that remained crystalline. The model is particularly effective for low shock levels, while Raman is more effective at higher shock pressures. These quantitative relationships provide a valuable tool for assessing the shock history recorded in plagioclase minerals.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 5","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143939533","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":"Formation of Pancake Domes on Venus as Viscous Flows Over an Elastic Lithosphere","authors":"M. E. Borrelli,&nbsp;C. Michaut,&nbsp;J. G. O'Rourke","doi":"10.1029/2024JE008571","DOIUrl":"https://doi.org/10.1029/2024JE008571","url":null,"abstract":"<p>Venus' steep-sided domes are circular volcanoes ∼10s of km wide and ∼1 km tall, which are known for their characteristic flat tops and steep sides. However, their composition remains mysterious. These “pancake” domes are likely formed by a high-viscosity lava, and other studies have predicted a range of compositions, from rhyolite to basalt. In this study, we build on previous work modeling pancake domes as spreading viscous gravity currents. However, previous models of dome formation assumed that they form over a rigid lithosphere. We previously found signatures of lithospheric flexure at 14 out of 75 pancake domes and therefore built a new model of dome formation over a bending elastic lithosphere. We found that flexure during formation can influence the shape of the resulting pancake dome. Our results also support the idea that pancake domes continue to spread for a long time after their emplacement. In comparing our model to the topography of a real pancake dome (Narina Tholus), we find a range of high, though variable, lava viscosities. Our range of lava viscosities is related to the size of the observed dome, and our results for a large dome agree with those of other studies. We test different lava densities and find that a lava density of ∼2,400–2,700 kg/m³ best reproduces the flexural signatures observed at Narina Tholus. Low-density lava (∼1,500 kg/m³) does not reproduce the flexural signatures, implying that dome-forming lava is not highly vesiculated.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 5","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-05-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008571","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930224","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 Map of Potential Topographic Anomalies on Venus","authors":"Gerard Gallardo i Peres,&nbsp;Philippa J. Mason,&nbsp;Richard C. Ghail","doi":"10.1029/2024JE008778","DOIUrl":"https://doi.org/10.1029/2024JE008778","url":null,"abstract":"<p>The most recent, highest-resolution, global estimate of the topography of Venus is the Global Topographic Data Record (GTDR), a gridded representation of the altimetry data from the Magellan space mission. This product is impaired by an occasional pattern; a series of visually striking topographic “pits,” often referred to as spuriously low values, which in many cases might be generating false topographic signatures. These generally arise from the incorrect identification of secondary, delayed power peaks in the individual altimeter records, which causes local topographic underestimations. There are many such “pits” across the GTDR, and they can lead to misinterpretation of geomorphological features. In this study, we describe GTDR data errors in detail and the situations in which they occur, and propose a method to classify spuriously low values across the entire product as potential anomalies. The method is based on the computation of the local altimeter ambiguity height around each pixel, modulated by an estimate of the relative elevation uncertainty between the pixel and the neighboring topography. We generate global maps of the potential anomalies, and find that up to 2.865% of the original product is impaired by them. They are concentrated in particular around rift systems and summit areas at low latitudes, and can be used to identify areas that would benefit from reprocessing the altimeter records. We argue that GTDR-supported geomorphological interpretations of surface features on Venus, in particular of <i>chasmata</i>, are susceptible to depth overestimation and cross-section distortion due to the accumulation of potential topographic anomalies.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 5","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-05-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008778","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930225","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 Role of the Magnetic Field Orientation on the Variability of the Martian Topside Ionosphere Using MARSIS-Mars Express Data","authors":"Dikshita Meggi,&nbsp;Beatriz Sánchez-Cano,&nbsp;Mark Lester,&nbsp;Simon Joyce,&nbsp;Katerina Stergiopoulou,&nbsp;Catherine Regan,&nbsp;David Andrews,&nbsp;Shaosui Xu,&nbsp;Xiaohua Fang,&nbsp;Olivier Witasse,&nbsp;Christopher M. Fowler","doi":"10.1029/2024JE008667","DOIUrl":"https://doi.org/10.1029/2024JE008667","url":null,"abstract":"<p>Mars, without a global dipole magnetic field, has its atmosphere directly exposed to the impinging solar wind, producing a complex interaction due to the remnant crustal magnetic fields, which, especially in the southern hemisphere, have spatially varying strengths and inclinations. “Mini-magnetospheres” generated over the strong crustal field regions, along with the planet's rotation, increase the complexity of ionosphere dynamics. This study analyses 28 Mars Express orbits spanning 12 years of observations from the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) instrument to characterize the variability of topside electron density profiles over strong crustal field anomalies in the southern hemisphere and far away from them. Variations are evaluated by quantifying the amount by which the electron density and total electron content depart from model fits assuming a Chapman layer. Regions of enhanced electron density, or topside layers, predominantly form during low solar activity both over and far from crustal field regions, indicating a solar cycle dependence. We find that topside layers are mostly confined to regions where crustal fields have horizontal inclinations or undergo drastic changes in orientation from vertical to horizontal. Moreover, the most horizontally extensive transient topside layers, spanning up to ∼33° latitude, are observed over unmagnetized regions dominated by draped horizontal magnetic fields. It is found that the total electron content on the dayside is enhanced by 12.5% in regions with horizontal magnetic fields and decreased by 15.0% where the fields are near-vertical.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 5","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-05-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008667","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143925944","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Characterizing the Facies and Stratigraphy of the Enchanted Lake Area in Jezero Crater, Mars","authors":"Michelle Tebolt,&nbsp;Kathryn M. Stack,&nbsp;Timothy A. Goudge,&nbsp;Libby R. W. Ives,&nbsp;Sanjeev Gupta,&nbsp;Gwénaël Caravaca,&nbsp;Robert Barnes,&nbsp;Gerhard Paar,&nbsp;Nicholas Randazzo","doi":"10.1029/2023JE008278","DOIUrl":"https://doi.org/10.1029/2023JE008278","url":null,"abstract":"<p>Jezero crater contains a sedimentary fan deposit previously interpreted as a delta, which can be studied to better understand the aqueous history of Mars. After a year of traversing and sampling the crater floor, the Mars 2020 <i>Perseverance</i> rover encountered the Enchanted Lake area at the base of the sedimentary fan. Data were collected at Enchanted Lake between sols ∼420–426 and again between sols 556–629 when the rover returned for sampling. The goal of this paper is to describe and characterize the facies within this outcrop to help constrain the paleoenvironment of Enchanted Lake in the context of the overall fan system. Facies are defined based on observed sedimentary structures, bedding geometries, and grain size. The lack of extensive cross-stratification combined with an abundance of soft sediment deformation, planar bedding, and normal grading leads us to interpret Enchanted Lake as a turbidite succession formed in a generally unconfined prodelta environment. Such depositional environments have high preservation potential for organic matter and potential biosignatures. Samples from these rocks have been collected by <i>Perseverance</i> for a planned Mars Sample Return mission. Our interpretation of Enchanted Lake is also consistent with other sedimentary deposits in the Jezero crater, such as the Kodiak butte, which is interpreted as deltaic in origin. Placing Enchanted Lake in context with Kodiak provides some constraints on the relative timing of these deposits within the Jezero fan system.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 5","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143925754","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":"Characterizing Extreme Compositions on the Moon Using Thermal Infrared Spectroscopy","authors":"Nandita Kumari,&nbsp;Laura B. Breitenfeld,&nbsp;Katherine Shirley,&nbsp;Timothy D. Glotch","doi":"10.1029/2024JE008814","DOIUrl":"https://doi.org/10.1029/2024JE008814","url":null,"abstract":"<p>The ultramafic and silicic rocks on the lunar surface have played an important role in expanding our knowledge regarding its thermal and magmatic evolution. The surface identification and quantification of these rocks on the global scale can significantly improve our understanding of their spatial extents, relationships and formation mechanisms. Christiansen feature positions using Diviner data have aided in global identification and mapping of relatively silica-rich and silica-poor lithologies on the lunar surface. We have used laboratory thermal infrared spectra of silicic and ultramafic rocks to analyze the variation in Christiansen feature in simulated lunar environment. We have characterized the absolute bulk silica content of the rocks and minerals and their Silica, Calcium, Ferrous iron, Magnesium index. We find that they are linearly correlated to the Christiansen feature despite particle size variations. Furthermore, we find that the Christiansen feature shifts toward longer wavelengths with increase in ilmenite content in the ilmenite-basalt mixtures. We have explored the effect of instrument's spectral band position on the accuracy of the parabolic method that is currently used for the estimation of Christiansen feature position from Diviner data. We find that this method performs poorly for the estimation of the Christiansen feature for ultramafic and silicic rocks and minerals/mineral mixtures. We propose using a machine learning algorithm to estimate the Christiansen feature with higher accuracy for all kinds of silicate compositions on the Moon. This method will lead to increased accuracy in absolute quantification of bulk silicate composition of the lunar surface at varying spatial scales.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 5","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143914269","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":"Mid-Infrared Reflectance and Emissivity Spectra of High Porosity Regoliths","authors":"Audrey C. Martin,&nbsp;Joshua P. Emery,&nbsp;Mark Loeffler,&nbsp;Kerri L. Donaldson Hanna","doi":"10.1029/2024JE008331","DOIUrl":"https://doi.org/10.1029/2024JE008331","url":null,"abstract":"<p>Mid-infrared (MIR; 5–35 μm) spectroscopy is often used for mineralogical identification on planetary surfaces. Laboratory spectra aiding remote sensing observations are typically performed in reflection geometries, while MIR spectra of planetary surfaces are typically obtained via emission. Here we explore the validity of Kirchhoff's Law in converting reflectance to emissivity spectra, focusing on the high-porosity regoliths found on airless bodies such as the Moon and asteroids. Specifically, we compared ambient reflectance, ambient emissivity, and simulated asteroid environment (SAE) spectra of fine-particulate olivine and pyroxene with varying regolith porosities, focusing on how spectral features, including the Christiansen feature (CF), reststrahlen bands (RBs), and transparency features (TF), changed under these different conditions. Our results indicate that Kirchhoff's Law can be effectively employed to interpret 19 MIR reflectance spectra of high-porosity samples, provided environmental spectral effects (i.e., spectral changes due to different pressure and temperature conditions) are considered.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 5","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008331","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143919606","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":"Coronae on Venus: An Updated Global Database and Insights Into Morphology, Spatial Distribution, Geological Setting, and Lithospheric Properties","authors":"A. J. P. Gülcher,&nbsp;L. Sabbeth,&nbsp;E. Stofan,&nbsp;S. E. Smrekar","doi":"10.1029/2024JE008749","DOIUrl":"https://doi.org/10.1029/2024JE008749","url":null,"abstract":"<p>Venus' surface hosts many volcanic and tectonic features, among which coronae are widespread. Despite their inferred significance for Venus' geodynamics, existing corona databases have been incomplete and/or inaccessible. Here, we present an updated database of coronae, which integrates and validates existing data sets while incorporating new insights. We define coronae using the criteria: (a) presence of a (partial/full) annulus of closely spaced concentric fractures, (b) with or without corresponding quasi-circular topographic relief, and (c) a minimum diameter of 60 km. Using this systematic approach, our database includes 740 corona features. We assess 507 to be Type 1 (fracture annuli <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>≥</mo>\u0000 </mrow>\u0000 <annotation> ${ge} $</annotation>\u0000 </semantics></math>180°) and 233 as Type 2 (fracture annuli <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>&lt;</mo>\u0000 </mrow>\u0000 <annotation> ${&lt; } $</annotation>\u0000 </semantics></math>180°) coronae. We identify subsets that share morphological traits with specific volcanic structures: 26 coronae show fracture annuli around domal shield volcanoes (Mons), and 112 features resemble large, collapsed caldera volcanoes or paterae. We also recognize a separate 46 “inter-tessera corona-like features” within the complex tesserae, which share similar morphological characteristics and have received little previous attention. We provide an analysis of the spatial distribution of coronae and examine their geological setting, topographic profiles, and lithospheric properties. We establish 11 topographic groups that can describe the diverse coronae. 26.4% of coronae display an elevated rim surrounding a depressed interior, while over 20% feature a full or partial trough. By linking the lithospheric and geological properties with corona morphologies, our study offers a deeper understanding of the diversity of coronae. Ultimately, this database provides a foundation for future investigations into the planet's geological evolution and surface activity.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 5","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008749","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143914122","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":"Geomorphological Evidence of Near-Surface Ice at Candidate Landing Sites in Northern Amazonis Planitia, Mars","authors":"Erica Luzzi,&nbsp;Jennifer L. Heldmann,&nbsp;Kaj E. Williams,&nbsp;Giacomo Nodjoumi,&nbsp;Ariel Deutsch,&nbsp;Alexander Sehlke","doi":"10.1029/2024JE008724","DOIUrl":"https://doi.org/10.1029/2024JE008724","url":null,"abstract":"<p>This work presents geomorphological analyses of an area at the boundary between Arcadia Planitia and northern Amazonis Planitia, situated in the northern mid-latitudes of Mars. Recent studies have indicated the presence of substantial volumes of near-surface excess ice in Arcadia Planitia, making this region a promising candidate for future human and robotic exploration. This study focuses on three specific candidate landing sites adjacent to the Arcadia Planitia: AP-1, AP-8, and AP-9. We have identified a wide range of ice-related morphologies, providing further evidence for the occurrence of excess ice in the study area. We have mapped and measured ∼9,000 thermal contraction polygons. We estimate ice beneath these polygons to be on the order of tens of cm from the surface, which is sufficiently shallow to be accessible for potential in situ resource utilization (ISRU). Recent impact craters that have been excavated into ice further suggest the presence of near-surface ice. Finally, the occurrence of ice and processes such as ice sublimation are likely responsible for the formation and subsequent modification of several observed features, including expanded craters, brain coral terrain, arcuate ridges, and thermal contraction polygons modified by sublimation. These results provide valuable insights into the ice distribution in the northern mid-latitudes and support the potential utilization of accessible ice resources for future human exploration efforts.</p>","PeriodicalId":16101,"journal":{"name":"Journal of Geophysical Research: Planets","volume":"130 5","pages":""},"PeriodicalIF":3.9,"publicationDate":"2025-05-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JE008724","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143901098","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}