Icarus最新文献

{"title":"The depletion of the asteroid belt and the impact history of the Earth","authors":"Julio A. Fernández","doi":"10.1016/j.icarus.2025.116824","DOIUrl":"10.1016/j.icarus.2025.116824","url":null,"abstract":"<div><div>We have evaluated the rate at which the asteroid belt is losing material, and how it splits between macroscopic bodies and meteoritic dust. The mass loss process is due to the injection of asteroid fragments into unstable dynamical regions, associated to mean-motion resonances with Jupiter, Saturn and Mars or secular resonances, from where they are scattered either to the region of the terrestrial planets or to the vicinity of Jupiter’s orbit. Asteroid fragments that do not escape from the belt are ground down by mutual collisions to meteoritic dust. Under the assumption that 25% of the zodiacal dust mass is of asteroidal origin, we find that the asteroid belt is currently losing a fraction of about <span><math><mrow><msub><mrow><mi>μ</mi></mrow><mrow><mi>o</mi></mrow></msub><mo>≃</mo><mn>8</mn><mo>.</mo><mn>8</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>5</mn></mrow></msup></mrow></math></span> Ma⁻¹ of its collisionally-active mass (without the primordial objects Ceres, Vesta and Pallas), about 20% as macroscopic bodies, and 80% as dust particles that feed the zodiacal dust cloud. Extrapolation of the current mass loss rate to the past suggests only a moderate increase of the asteroid belt mass and the mass loss rate around 3.0−3.5 Ga ago (by about 50% and a factor of two respectively). Yet, should the computed <span><math><msub><mrow><mi>μ</mi></mrow><mrow><mi>o</mi></mrow></msub></math></span> be somewhat underestimated owing to the different uncertainties associated to its computation, the extrapolation to the past would lead to quite different results. For instance, a moderate increase in the computed <span><math><msub><mrow><mi>μ</mi></mrow><mrow><mi>o</mi></mrow></msub></math></span>, say by a factor of three, would lead to an exponential increase of the asteroid mass and mass loss rate about 3.5 Ga ago. A greater asteroid mass loss rate in the past should be correlated with a more intense impact rate of the Earth, Moon and the other terrestrial planets, which is indeed what suggests the geologic record (Hartmann et al., 2007).</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116824"},"PeriodicalIF":3.0,"publicationDate":"2025-09-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145157399","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"High-altitude Martian plume is likely an ordinary twilight cloud","authors":"M.M.J. Crismani ,&nbsp;M.S. Chaffin ,&nbsp;K. Connour ,&nbsp;N.M. Schneider ,&nbsp;S. Curry ,&nbsp;J. Deighan ,&nbsp;R. Fitzpatrick ,&nbsp;S. Jain ,&nbsp;G. Liuzzi ,&nbsp;M. Slipski ,&nbsp;G.L. Villanueva","doi":"10.1016/j.icarus.2025.116823","DOIUrl":"10.1016/j.icarus.2025.116823","url":null,"abstract":"<div><div>Sánchez-Lavega et al. (2015) analyzed ground-based and space-based images of Mars that they interpreted as showing two high-altitude plumes. Their derived plume altitudes of 200 to 250 km or higher defied atmospheric processes known at the time. No supporting observations have been published in the decade since, despite ample observations by the fleet of spacecraft currently orbiting the planet. Instead, more recent observations provide strong constraints against the interpretations proposed at the time. We therefore reanalyzed the images used in that work and reviewed the methods employed by Sánchez-Lavega et al. (2015). We have identified several issues in the original data processing that may have affected the altitude determination, including surface-feature registration, black-level selection, color-image alignment, inconsistent map gridding, unknown image preprocessing, and the propagation of systematic uncertainties. Our independent analysis indicates that the features in these images are consistent with post-terminator clouds with altitudes between 50 and 100 km. Such clouds are relatively common at Mars and require no new atmospheric physics or chemistry to understand.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"444 ","pages":"Article 116823"},"PeriodicalIF":3.0,"publicationDate":"2025-09-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145156180","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Milankovitch forcing of equilibrium ground-ice on Mars","authors":"Oded Aharonson ,&nbsp;Eran Vos ,&nbsp;Ehouarn Millour ,&nbsp;Francois Forget ,&nbsp;Norbert Schörghofer","doi":"10.1016/j.icarus.2025.116772","DOIUrl":"10.1016/j.icarus.2025.116772","url":null,"abstract":"<div><div>Exchangeable ice deposits are present today on the surface of Mars in polar caps and in the shallow subsurface in mid-latitudes. Geologic observations indicate these deposits waxed and waned in the past, at times, along with the emplacement and loss of equatorial glaciers. Here, we couple a climate model with an ice stability criterion, to self-consistently determine the distribution of the mid-latitude ground-ice deposits in diffusive equilibrium with the atmosphere, at present and under past orbital configurations. This new coupling and iteration between the short-term and long-term models improves upon past calculations that do not allow the ice table to evolve over timescales much longer than the annual climate dynamics. The model predictions for the extent of the equilibrium ice-table in the past match the latitudinal distribution of terrain softening geologic features previously mapped. At past times, thermally stable shallow ground ice is expected even in equatorial regions, in parts of Tharsis and Arabia Terra.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"444 ","pages":"Article 116772"},"PeriodicalIF":3.0,"publicationDate":"2025-09-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145119734","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Erratum to ‘Rock suites of Endeavour crater, Mars: Comparing Perseverance Valley, Spirit of St. Louis, and Marathon Valley’ Icarus 442C (2025) 116752","authors":"Michael C. Bouchard,&nbsp;Bradley L. Jolliff","doi":"10.1016/j.icarus.2025.116805","DOIUrl":"10.1016/j.icarus.2025.116805","url":null,"abstract":"","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"444 ","pages":"Article 116805"},"PeriodicalIF":3.0,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145097714","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Mineral quantitative inversion based on in-situ spectral observations from Yutu-2: Anomalous sample origin and mineral composition variations on the Rover's path","authors":"Kecheng Du ,&nbsp;Sicong Liu ,&nbsp;Xiaohua Tong ,&nbsp;Qian Du ,&nbsp;Huan Xie ,&nbsp;Yongjiu Feng ,&nbsp;Yanmin Jin","doi":"10.1016/j.icarus.2025.116821","DOIUrl":"10.1016/j.icarus.2025.116821","url":null,"abstract":"<div><div>In January 2019, China's Chang'e-4 (CE-4) spacecraft successfully landed in Von Kármán crater on the farside of the Moon. During nearly six years of operation until November 2024, the Visible and Near-infrared Image Spectrometer (VNIS) onboard the Yutu-2 rover acquired in-situ spectral data along an approximately 1600 m traverse path, offering critical opportunities to investigate subtle mineralogical variations within the patrol region. In this study, we analyzed these spectral data using a sparse spectral decomposition method with TiO₂ constraints to quantitatively estimate the abundances of six lunar minerals, including high‑calcium pyroxene, low-calcium pyroxene, olivine, plagioclase, ilmenite and agglutinate/glass. We further examined the mineralogical properties of regolith and rocks in Yutu-2's patrol area to identify trends and correlations in compositional variations. By comparing results with Kaguya Multiband Imager data products, we identified a gradual decreasing spatial distribution in plagioclase abundance along the traverse path, likely attributable to ejecta from the Zhinyu crater. Furthermore, analysis of Moon Mineral Mapper (M³) data revealed samples with similar spectral characteristics near Zhinyu crater, supporting this hypothesis. Additionally, the impact of secondary impact craters on local regions was qualitatively and quantitatively assessed using VNIS spectral features and agglutinate/glass abundance. These findings enhance understanding of the complex origin and evolution of materials at the CE-4 landing site region.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"444 ","pages":"Article 116821"},"PeriodicalIF":3.0,"publicationDate":"2025-09-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145119733","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"A full-atmosphere model of Jupiter","authors":"Antonín Knížek ,&nbsp;Paul B. Rimmer ,&nbsp;Martin Ferus","doi":"10.1016/j.icarus.2025.116806","DOIUrl":"10.1016/j.icarus.2025.116806","url":null,"abstract":"<div><div>This paper presents a combined 1D photochemical–thermochemical kinetics model of Jupiter’s deeper atmosphere, troposphere and stratosphere. The model covers atmospheric pressure range from <span><math><mrow><mn>1</mn><mo>.</mo><mn>1</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>3</mn></mrow></msup></mrow></math></span> bar to <span><math><mrow><mn>7</mn><mo>.</mo><mn>4</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>11</mn></mrow></msup></mrow></math></span> bar and is the first model that incorporates sulfur chemistry when spanning an atmospheric region of this extent. This model incorporates a new version of the STAND reaction network with updated NH₄SH chemistry, and updated Antoine equation parameters for NH₄SH and H₂S. Validation against current models of Jupiter’s atmosphere as well as recent observational data shows that our model successfully describes Jupiter’s main observed chemical features. Since one of the focuses of the model is the chemistry on nitrogen, it correctly predicts the formation of a mixed NH₃-NH₄SH cloud layer between 0.1 and 1 bar. It also describes the chemistry of HCN throughout the atmosphere and discovers a region in the stratosphere between <span><math><mrow><mn>1</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>6</mn></mrow></msup></mrow></math></span> and <span><math><mrow><mn>6</mn><mo>.</mo><mn>76</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>8</mn></mrow></msup></mrow></math></span> bar, where HCN forms through radical chemistry with maximum mixing ratio 33 ppb at <span><math><mrow><mn>2</mn><mo>.</mo><mn>94</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>7</mn></mrow></msup></mrow></math></span> bar – a prediction testable by observations. At the same time, our model predicts a quenched N₂ mixing ratio 490 ppm up to 10⁻⁶ bar. The model therefore successfully bridges the gap between existing models of separate regions of Jupiter’s atmosphere and makes new testable predictions of several chemical species.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"444 ","pages":"Article 116806"},"PeriodicalIF":3.0,"publicationDate":"2025-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145156179","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Noble gas fractionation predictions for high speed sampling in the upper atmosphere of Venus","authors":"Arnaud Borner ,&nbsp;Michael A. Gallis ,&nbsp;Rita Parai ,&nbsp;Guillaume Avice ,&nbsp;Mihail P. Petkov ,&nbsp;Krishnan Swaminathan-Gopalan ,&nbsp;Christophe Sotin ,&nbsp;Jason Rabinovitch","doi":"10.1016/j.icarus.2025.116800","DOIUrl":"10.1016/j.icarus.2025.116800","url":null,"abstract":"<div><div>Venus, our neighboring planet, is an open-air laboratory that can be used to study why Earth and Venus evolved in such different ways and even to better understand exoplanets. Noble gases in planetary atmospheres are tracers of their geophysical evolution, and measuring the elemental and isotopic composition of noble gases in the Venus atmosphere informs us about the origin and evolution of the entire planet. In this work we describe a new mission concept, Venus ATMOSpheric - Sample Return (VATMOS-SR), that would return gas samples from the upper atmosphere of Venus to Earth for scientific analysis. This could be the first sample return mission for an extraterrestrial atmosphere. To ensure it is possible to relate the composition of the sampled gases (acquired when the spacecraft is traveling <span><math><mrow><mo>&gt;</mo><mn>10</mn></mrow></math></span> km/s) to the freestream atmospheric composition, large-scale numerical simulations are employed to model the flow into and through the sampling system. In particular, an emphasis is placed on quantifying noble gas elemental and isotopic fractionation that occurs during the sample acquisition and transfer process, to determine how measured isotopic ratios of noble gases in the sample would compare to the actual isotopic ratios in the Venusian atmosphere. We find that lighter noble gases are depleted after they are sampled compared to the freestream conditions, and heavier ones are enriched, due to the high pressure gradients present in the flowfield. We also observe that lighter noble gases are more affected than heavier ones by changes in the freestream conditions. Finally, we observe that, in general, the numerical parameters do not have a major impact on the observed fractionation. We do, however, note that the freestream velocity and density have a major impact on fractionation, and do need to be precisely known to properly reconstruct the fractionation in the sampling system. We demonstrate that the sample fractionation can be predicted with numerical simulations, and believe that VATMOS-SR, which could be the first mission to bring back samples from another planet, could answer key scientific questions related to understanding the evolution of Venus.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"444 ","pages":"Article 116800"},"PeriodicalIF":3.0,"publicationDate":"2025-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145119706","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Detailed topographic and geomorphological analyses of Chang'e-6 landing area","authors":"Yexin Wang ,&nbsp;Chenxu Zhao ,&nbsp;Biao Wang ,&nbsp;Bin Xie ,&nbsp;Kaichang Di ,&nbsp;Hong Zhang ,&nbsp;Xiangjin Deng ,&nbsp;Wai Chung Liu ,&nbsp;Yifan Zhang ,&nbsp;Bin Liu ,&nbsp;Ruiqing Sheng ,&nbsp;Yang Zhao ,&nbsp;Shujuan Sun ,&nbsp;Li Li ,&nbsp;Sheng Gou ,&nbsp;Zongyu Yue","doi":"10.1016/j.icarus.2025.116820","DOIUrl":"10.1016/j.icarus.2025.116820","url":null,"abstract":"<div><div>China's Chang'e-6 (CE-6) mission landed successfully in the Apollo basin inside the South Pole-Aitken basin, marking the first lunar farside sample return mission. Prior to the landing of the probe, detailed analyses of the topography and geomorphology of the target landing area are necessary to ensure a safety landing. This paper presents the approaches and results of topographic and geomorphological analyses for the 28 km × 6 km pre-selected landing area of the CE-6 mission. First, a seamless digital orthophoto map (DOM) of the area with resolution of 1 m/pixel is produced using the Lunar Reconnaissance Orbiter Narrow Angle Camera images. Second, a 1 m/pixel resolution digital elevation model (DEM) of this area is generated based on the deep learning terrain reconstruction method, and topographic analysis is conducted based on the DEM. Third, on the basis of the DOM and DEM data, typical geomorphological features within the pre-selected landing area, such as craters and rocks, are extracted and their properties are analyzed. The above topographic data and analyses results directly supported detailed landing site selection and safe landing for the CE-6 mission, and provide fundamental information for further scientific investigations of the landing area and the collected samples.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"444 ","pages":"Article 116820"},"PeriodicalIF":3.0,"publicationDate":"2025-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145156178","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Numerical simulation of asteroid geometry variance on airburst threat","authors":"Sean P. Stokes ,&nbsp;Jason M. Pearl ,&nbsp;Veronika A. Korneyeva ,&nbsp;J. Michael Owen ,&nbsp;Cody Raskin ,&nbsp;Arihant Jain ,&nbsp;Javid Bayandor","doi":"10.1016/j.icarus.2025.116819","DOIUrl":"10.1016/j.icarus.2025.116819","url":null,"abstract":"<div><div>For an atmospheric airburst the primary source of concern when assessing uncertainty is the size and velocity. Determining these properties provides the basis for threat assessment, as the total energy of the asteroid may then be estimated, and the threat investigated thoroughly. Even with clarity as to how much energy an asteroid may deposit, a great deal of uncertainty still exists for the actual energy deposition process. One such source of uncertainty is the geometry of the incoming asteroid. The geometry of an asteroid will alter the stress distribution during entry, which adds uncertainty to when fracture will occur. In this study, we use Smoothed Particle Hydrodynamics to model the atmospheric airburst of Tunguska-scale asteroids with varying geometric profiles, including a sphere, ellipsoid, binary and superellipsoid. Each asteroid is modeled as a homogenous structure with strength. We assess uncertainty through a series of planar 2D simulation cases for each geometry, comparing the source of stochasticity across geometries. A single 3D airburst simulation for each geometry is also analyzed. Additionally, the 3D cases are compared to the highly uncertain Tunguska event, predicting variance in burst height across geometries, but all bounded by theoretical burst heights proposed for Tunguska.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"444 ","pages":"Article 116819"},"PeriodicalIF":3.0,"publicationDate":"2025-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145097720","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Convective flow in Ganymede’s subsurface ocean: Implications for the induced magnetic field and topography","authors":"Jakub Kvorka,&nbsp;Ondřej Čadek,&nbsp;Libor Šachl,&nbsp;Jakub Velímský","doi":"10.1016/j.icarus.2025.116807","DOIUrl":"10.1016/j.icarus.2025.116807","url":null,"abstract":"<div><div>Subsurface oceans of icy moons are inaccessible to direct observation and numerical modeling is currently the only way to study the dynamics of these systems. Here, we present the first comprehensive study of Ganymede’s ocean based on the numerical simulations of thermal convection in a rotating spherical shell, and discuss the implications of the flow circulation for Ganymede’s long-wavelength topography and induced magnetic field. In order to determine the structure of the flow in Ganymede’s ocean, we have performed 128 numerical simulations, varying all relevant control parameters (<span><math><mrow><mi>R</mi><mi>a</mi></mrow></math></span>, <span><math><mrow><mi>E</mi><mi>k</mi></mrow></math></span>, <span><math><mrow><mi>P</mi><mi>r</mi></mrow></math></span>) by at least one order of magnitude. Based on this data set, we predict that the ocean circulation is characterized by a retrograde equatorial jet, meridional circulation cells at low latitudes and narrow upwellings and downwellings in the polar regions. The mean speed of the ocean flow ranges from a few cm/s for a thin (<span><math><mrow><mo>&lt;</mo><mspace></mspace><mn>100</mn></mrow></math></span> km) ocean to 0.8<!--> <!-->m/s for a 500<!--> <!-->km thick ocean. The time-averaged heat flux from the ocean varies with the latitude reaching the maximum at the poles and the minimum at mid-latitudes. Assuming that the heat transfer in the ice shell is dominated by conduction, we determine Ganymede’s long-wavelength topography generated by the uneven heat flux from the ocean. We predict that Ganymede’s polar regions are flat or even elevated and the global topographic pattern is dominated by an equatorial depression and elevations at mid-latitudes. Preliminary calculations of the magnetic field, induced by the flow of the salty ocean in the presence of Ganymede’s internal magnetic field, predict sufficiently large amplitudes to allow their detection by the Juice and Europa Clipper spacecrafts. We demonstrate that the pattern of the flow-induced magnetic field strongly depends on the geometry of ocean circulation, suggesting that accurate magnetic measurements can provide constraints on the dynamics of Ganymede’s ocean.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"444 ","pages":"Article 116807"},"PeriodicalIF":3.0,"publicationDate":"2025-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145119707","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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}