Planetary and Space Science最新文献

{"title":"High-resolution rock abundance derivation of lunar cold spot craters based on RA-SAR model","authors":"Jiacheng Sun ,&nbsp;Xin Lu ,&nbsp;Gaofeng Shu ,&nbsp;Zhengwei Guo ,&nbsp;Ning Li","doi":"10.1016/j.pss.2025.106138","DOIUrl":"10.1016/j.pss.2025.106138","url":null,"abstract":"<div><div>The distribution of rock abundance (RA) on the lunar surface plays a pivotal role in understanding its geological evolution. This study focuses on the derivation of high-resolution RA data for lunar cold spot craters using Mini-RF (Miniature Radio Frequency) synthetic aperture radar (SAR) data. Firstly, terrain correction was applied to the SAR data. Secondly, the correlation between the Stokes parameters (<span><math><mrow><msub><mi>S</mi><mn>1</mn></msub></mrow></math></span>, <span><math><mrow><msub><mi>S</mi><mn>2</mn></msub></mrow></math></span>, <span><math><mrow><msub><mi>S</mi><mn>3</mn></msub></mrow></math></span>, and <span><math><mrow><msub><mi>S</mi><mn>4</mn></msub></mrow></math></span>) and RA was examined using optically-derived RA data, which aligns with the resolution of the Mini-RF SAR images. By plotting scatter diagrams showing the relationships between the Stokes parameters and the optically-derived RA, strong statistical associations were established. Finally, based on these findings, we formulated a regression-based RA-SAR model. This model was applied to other lunar cold spot craters in order to derive their high-resolution RA distributions. The experimental results show that the model yields highly precise outcomes when validated against both Diviner RA and optical data. The study provides a new approach for inferring rock distribution across the lunar surface using SAR data, and offers valuable insights for advancing lunar geological research.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"263 ","pages":"Article 106138"},"PeriodicalIF":1.8,"publicationDate":"2025-05-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144134158","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Dynamical regimes of two eccentric and mutually inclined giant planets","authors":"Tabare Gallardo,&nbsp;Alfredo Suescun","doi":"10.1016/j.pss.2025.106137","DOIUrl":"10.1016/j.pss.2025.106137","url":null,"abstract":"<div><div>We consider a basic planetary system composed by a Sun like star, a Jupiter-like planet and a Neptune-like planet in a wide range of orbital configurations not limited to the hierarchical case. We present atlases of resonances showing the domains of <span><math><mo>∼</mo></math></span> <span><math><mrow><mn>1300</mn></mrow></math></span> mutual mean-motion resonances (MMRs) and their link to chaotic and regular dynamics. Following a semi-analytical method for the study of the secular dynamics we found two regimes for equilibrium configurations: one for low mutual inclinations were equilibrium is related to oscillations of <span><math><mrow><mi>Δ</mi><mi>ϖ</mi></mrow></math></span> around <span><math><mrow><mn>0</mn><mo>°</mo></mrow></math></span> or <span><math><mrow><mn>180</mn><mo>°</mo></mrow></math></span>, and other for high mutual inclinations where the equilibrium is given by defined values of the <span><math><msub><mrow><mi>ω</mi></mrow><mrow><mi>i</mi></mrow></msub></math></span> equal to integer multiples of <span><math><mrow><mn>90</mn><mo>°</mo></mrow></math></span>. By numerical integration of the full equations of motion we calculate the fundamental frequencies of the systems in their diverse configurations and study their dependence with the orbital elements. According to the analysis of the fundamental frequencies we found two dynamical regimes depending on the initial mutual inclination and the limit between the two regimes occurs at some critical inclination <span><math><mrow><mn>30</mn><mo>°</mo><mo>≲</mo><msub><mrow><mi>i</mi></mrow><mrow><mi>c</mi></mrow></msub><mo>≲</mo><mn>40</mn><mo>°</mo></mrow></math></span> defined by the occurrence of the secular resonance <span><math><mrow><msub><mrow><mi>g</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><msub><mrow><mi>g</mi></mrow><mrow><mn>2</mn></mrow></msub></mrow></math></span>. For <span><math><mrow><mi>i</mi><mo>&lt;</mo><msub><mrow><mi>i</mi></mrow><mrow><mi>c</mi></mrow></msub></mrow></math></span> the dynamics is analogue to the classic secular model for low <span><math><mrow><mo>(</mo><mi>e</mi><mo>,</mo><mi>i</mi><mo>)</mo></mrow></math></span> with well defined three fundamental frequencies and free and forced modes, conserving quasi constant the mutual inclination. For <span><math><mrow><mi>i</mi><mo>&gt;</mo><msub><mrow><mi>i</mi></mrow><mrow><mi>c</mi></mrow></msub></mrow></math></span> the dynamics is completely different with increasing changes in mutual inclination and emerging combinations of the fundamental frequencies and, depending on the case, dominated by the secular resonance or the vZLK mechanism.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"263 ","pages":"Article 106137"},"PeriodicalIF":1.8,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144107605","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Sealing Europa’s vents by vapor deposition: An order-of-magnitude study","authors":"S. Boccelli ,&nbsp;S.R. Carberry Mogan ,&nbsp;R.E. Johnson ,&nbsp;O.J. Tucker","doi":"10.1016/j.pss.2025.106136","DOIUrl":"10.1016/j.pss.2025.106136","url":null,"abstract":"<div><div>Fractures and vents in the ice crust of Europa, exposing the sub-surface ocean or liquid–water inclusions to the vacuum, might be responsible for the generation of water-vapor plumes. During its passage through the ice, the plume vapor is expected to partially condense on the cold ice walls. Together with other effects (water spillage, compression forces, etc.) this mechanism likely contributes to sealing the vent. In this work, we develop a simple lumped-parameter model that can quantify how quickly a hypothetical vent of prescribed width would be sealed via water-vapor deposition. As an example, we apply our model to the vent size and density conditions inferred from the 2012 Hubble Space Telescope plume detection, predicting a sealing time of about 30 min. This suggests that the actual ice fracture might have been larger than originally proposed and/or the plume density at the vent might have been lower. While many other effects could have been present and responsible for sealing the vent, our estimates indicate that vapor deposition might have played a major role in eventually shutting off the observed plume. A map of sealing times vs. plume density, mass flow rate and aperture areas is given. Plume quantities from the literature are analyzed and compared to our results. For a given plume density/mass flow rate, small apertures would be sealed quickly by vapor deposition and are thus incompatible with observations.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"263 ","pages":"Article 106136"},"PeriodicalIF":1.8,"publicationDate":"2025-05-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144099488","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"On ore-bearing asteroid remnants in lunar craters","authors":"Jayanth Chennamangalam ,&nbsp;Paul Brook ,&nbsp;Martin Elvis ,&nbsp;Samuel Peterson","doi":"10.1016/j.pss.2025.106129","DOIUrl":"10.1016/j.pss.2025.106129","url":null,"abstract":"<div><div>We modify the probabilistic formalism developed by Elvis (2014) to estimate the number of lunar craters that contain ore-bearing asteroid remnants. When we consider craters at or above a threshold diameter of 1<!--> <!-->km, we estimate an upper limit of <span><math><mrow><mo>∼</mo><mn>6</mn><mo>,</mo><mn>500</mn></mrow></math></span> craters with asteroid remnants containing significant amounts of platinum group metals and an upper limit of <span><math><mrow><mo>∼</mo><mn>3</mn><mo>,</mo><mn>400</mn></mrow></math></span> craters with asteroid remnants that contain significant amounts of water in the form of hydrated minerals. For a more conservative threshold of 5<!--> <!-->km, we estimate <span><math><mrow><mo>≲</mo><mn>400</mn></mrow></math></span> craters with asteroid remnants that contain significant amounts of platinum group metals. These values are one to two orders of magnitude larger than the number of ore-bearing near-Earth asteroids estimated by Elvis (2014), implying that it may be more advantageous, and hence more profitable, to mine asteroids that have impacted the Moon rather than the ones that are in orbit.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"263 ","pages":"Article 106129"},"PeriodicalIF":1.8,"publicationDate":"2025-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144090097","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Measurement of bipolar charge distribution of lunar dust simulant under VUV irradiation","authors":"Rémi Pacaud ,&nbsp;Jean-Charles Matéo-Vélez ,&nbsp;Sébastien Hess ,&nbsp;Sylvain Ranvier","doi":"10.1016/j.pss.2025.106120","DOIUrl":"10.1016/j.pss.2025.106120","url":null,"abstract":"<div><div>Upcoming missions to the Moon represent new science opportunities and challenges. The electrostatic nature of the regolith combined with the solar wind makes it loft and adhere to almost any surface, which represents a threat for future manned and robotic missions. Understanding the charge state of the lunar soil under a representative environment is a key step towards ensuring safe lunar missions. While the global first order effect of exposure to the Sun's UV is to charge the soil positively, past experiments suggested that the transported dusts could be charged negatively. This counter-intuitive behavior was then supported by modeling, which explained the existence of negative charges but also predicted that of positively charged ones. To investigate the charging behavior of dust under a representative environment, we developed an experimental protocol based on a polarized sensitive sensor dedicated to the charge measurement of single dust grains with an accuracy of about 1 fC. The first set of measurements obtained with JSC-1A lunar dust simulants in high vacuum reveals the bipolar nature of lunar dust net charge in the regolith when exposed to UVs. Indeed, both positive and negative dusts were detected, supporting the complexity of the regolith charging processes suggested by the models.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"263 ","pages":"Article 106120"},"PeriodicalIF":1.8,"publicationDate":"2025-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143943182","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Using imagery from the Mars Science Laboratory mission to understand wind properties of aerosols aloft","authors":"C.L. Campbell ,&nbsp;J.E. Moores","doi":"10.1016/j.pss.2025.106119","DOIUrl":"10.1016/j.pss.2025.106119","url":null,"abstract":"<div><div>Since landing in 2012, the Mars Science Laboratory (MSL, Curiosity) has been investigating local aerosols through atmospheric imagery taken by its onboard Navigation Cameras (NCAMs). In particular, a Zenith Movie (ZM), is a vertically pointed 8-frame movie that is used to classify meteorological wind direction based on aerosol movement within the frames. Several Mars Year (MY) worth of data have been analysed and found repeatable wind directions year-to-year. Water-ice clouds in the Aphelion season had strong Easterly winds, which agrees with modelling that shows a strong cross-equatorial Hadley cell in this season. The Perihelion season did not show any strong directions, which was attributed to the chaotic motion seen in dust clouds expected during this season. When compared to the Rover Environmental Monitoring Station (REMS) onboard MSL, wind directions from the ZMs did not agree with REMS results. This mismatch between REMS and ZM wind results indicates that aerosols observed in imagery are most likely well above the crater rather than at the surface where REMS is located.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"263 ","pages":"Article 106119"},"PeriodicalIF":1.8,"publicationDate":"2025-05-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143947816","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The evolution of Nirgal Vallis (Mars) based on morphometric results: does tectonics play a role?","authors":"A. Szilágyi-Sándor,&nbsp;B. Székely","doi":"10.1016/j.pss.2025.106128","DOIUrl":"10.1016/j.pss.2025.106128","url":null,"abstract":"&lt;div&gt;&lt;div&gt;One of the unique valleys in the southern hemisphere of Mars is the 700 km long Nirgal Vallis. The catchment area of the river-like valley, presumably formed in the Hesperian period (3000–3700 Ma ago), has been shaped over time by many influences. The goal of this study is to explore and separate these potential influences including changes in the water level of the Uzboi Vallis, its erosion base. The other aim is to detect and describe the effects of tectonic processes for we have found potential evidence. Our working hypothesis is that Nirgal Vallis was once a river valley: our study analyses this possibility. The climate of Mars has undergone drastic changes in the past, and liquid water is currently not stable on the surface. The formation of former river valleys after the active wet period continued, including Nirgal Vallis. Morphometric techniques were applied based on MOLA, THEMIS, and HiRISE data. The topography of the Nirgal Vallis have been analyzed by swath analysis, calculation of various geomorphometric parameters, and runoff model. HiRISE digital terrain models having decimeter-scale resolution derived from the HiRISE stereopairs have been used for the detailed analysis.&lt;/div&gt;&lt;div&gt;A subdivision of the Nirgal Vallis according to its tectonic geomorphological structures was established. The swath analysis and the runoff model calculation show that, although the valley does not have a strict thalweg today, i.e., water currently cannot flow down it, the valley does have a trend of slope along the whole length and even intermittent slope changes can be observed along the whole valley. Several small-scale morphological features were also identified using MOLA data.&lt;/div&gt;&lt;div&gt;We conclude that the tectonic processes have transformed the morphology of the riverbed: it is divided into small sections (closed basins) so that currently water would not be able to flow down in it. Extraterrestrial (i.e. effects from outside Mars) causes on Mars also influence this, i.e. the formation of larger and smaller craters has also left its mark on the topography. We interpret the subperpendicular elongated morphological features on the plateau surrounding Nirgal Vallis as wrinkle ridges: their size, shape and spacing is similar to those identified by previous authors elsewhere. We also found evidence that the valley bottom has also been modified by the processes that formed the wrinkle ridges. Our observations imply younger tectonic influence of the area, presumably, postdating the fluvial erosional regime.&lt;/div&gt;&lt;div&gt;The Luki Crater, located near the confluence of Nirgal Vallis and Uzboi Vallis, has also been analyzed, and evidence has been found to be tectonically modified. This modification is in congruence with the results of other analyses indicating tectonic influence of Nirgal Vallis. Our results may also have implications for formation of the Uzboi Vallis, though this will require further studies.&lt;/div&gt;&lt;div&gt;These results suggest that the a","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"262 ","pages":"Article 106128"},"PeriodicalIF":1.8,"publicationDate":"2025-04-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143878449","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Absolute photometry of small main-belt binary asteroids. Physical properties","authors":"Vasilij G. Chiorny ,&nbsp;Yurij N. Krugly ,&nbsp;Vasilij G. Shevchenko ,&nbsp;Ivan G. Slyusarev ,&nbsp;Olga I. Mikhalchenko","doi":"10.1016/j.pss.2025.106118","DOIUrl":"10.1016/j.pss.2025.106118","url":null,"abstract":"<div><div>Here we present the physical characteristics of 24 discovered and 2 probable small binary asteroids at the inner main belt based on photometric lightcurves of the primary components of these systems obtained in the standard <em>VR</em> spectral bands, as well as the determination of the <em>V–R</em> color indices and the absolute magnitudes <em>H</em>_V of the studied objects. We also make estimates of the effective diameters of six asteroids which radiometric data are not available.</div><div>Analysis of the <em>V–R</em> color indices, revised albedo, color indices obtained from the SDSS and Sky-Mapper surveys, as well as recently published spectral characteristics in the visible and infrared wavelength ranges, allows us to effectively make a taxonomy of the observed asteroids. We have determined that the most of these primary components of the main-belt small binary asteroids belong to the moderate-albedo S-type with the mean albedo 0.24 ± 0.08. Also, there are moderate-albedo asteroids of the A, M, Q, and V-types as well as high-albedo E-type in our sample. It should be noted that asteroids with low albedo are absent in our set of binary asteroids.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"262 ","pages":"Article 106118"},"PeriodicalIF":1.8,"publicationDate":"2025-04-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143903466","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Understanding the effects of geotechnical properties on viscous erosion rate from plume surface interactions","authors":"B. Dotson,&nbsp;A. St John,&nbsp;R. Hall,&nbsp;D. Sapkota,&nbsp;D. Britt,&nbsp;P. Metzger","doi":"10.1016/j.pss.2025.106117","DOIUrl":"10.1016/j.pss.2025.106117","url":null,"abstract":"<div><div>With humans returning to the Moon under the Artemis program, understanding and mitigating effects from Plume Surface Interactions (PSI) will be essential for the protection of personnel and equipment on the Moon. To help characterize the underlying mechanics associated with viscous erosion and crater formation, experimental measurements using regolith simulants and subsonic, non-reacting flows were completed using compressed air in a splitter plate, plume cratering setup. More specifically, these investigations examined the underlying effects of bulk density, cohesion, and exhaust flow characteristics on viscous erosion rates and crater formation using Lunar highlands simulant (LHS-1), Lunar mare simulant (LMS-1), LHS-1D (Dust) simulants, and 40–80 μm glass beads in atmosphere. Results show that particle size distribution can ultimately influence crater shapes and erosion rates, likely owing to internal angle of friction. Measurements show that increasing bulk density, especially from an uncompacted to a slightly compacted state, decreases erosion rate by as much as 50 %. While cohesion of granular material can mitigate erosion rates to some extent, higher levels of cohesion above 1000 Pa may actually increase viscous erosion rates due to particle clumping. A modified version of Metzger's (2024a)equation for volumetric erosion rate is presented, with limitations discussed. These modified equations for viscous erosion, with limitations noted, show that geotechnical properties play an important role in viscous erosion and should be considered in PSI computer models for future mission planning.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"261 ","pages":"Article 106117"},"PeriodicalIF":1.8,"publicationDate":"2025-04-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143822359","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Automatic morphologic classification of Martian craters using imbalanced datasets of Tianwen-1’s MoRIC images with deep neural networks","authors":"Qifang Zheng ,&nbsp;Rong Huang ,&nbsp;Yusheng Xu ,&nbsp;Fangzhao Zhang ,&nbsp;Changjiang Xiao ,&nbsp;Luning Li ,&nbsp;Xiaohua Tong","doi":"10.1016/j.pss.2025.106104","DOIUrl":"10.1016/j.pss.2025.106104","url":null,"abstract":"<div><div>Martian impact craters contain prolific geomorphic information; their types provide vital indicators reflecting the geological evolution and chronology of celestial bodies. Currently, visual inspection is the most commonly used and widely accepted approach for identifying the crater types and their morphological features. However, it is a subjective task and requires professional knowledge. In this work, we present a method for the automatic morphologic classification of Martian craters using imbalanced Mars image datasets. Specifically, we classified and cropped Tianwen-1’s MoRIC images according to the morphological features of craters based on Robbins’ impact crater catalog; a dataset of six different types of Mars impact craters was established using the images. Based on this dataset, we classified the Mars impact craters using three popular neural network models with CNN and Transformer architectures. Meanwhile, to address the imbalanced samples in the network training process, a common problem in planetary remote sensing datasets, we introduce two methods (i.e., label smoothing strategy and weighted loss function) to suppress its influence on classification accuracy. Experimental results show that the Vision Transformer (ViT) model has the highest classification accuracy, reaching 90.3%. The label smoothing strategy performs well in CNN approaches, among which VGGNet11 improves the accuracy by 2.2%. By contrast, the weighted loss function performs well in ViT, and the classification accuracy of ViT improves by 1.3%. These results demonstrate a promising future for applying deep neural networks to identify and morphologically analyze Martian craters automatically.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"262 ","pages":"Article 106104"},"PeriodicalIF":1.8,"publicationDate":"2025-04-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143833259","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}