Icarus最新文献

{"title":"Interaction between oppositely signed vortices on adjacent domains in Jupiter","authors":"R. Morales-Juberías ,&nbsp;Liming Li ,&nbsp;Timothy Dowling ,&nbsp;Serenity Mercuri ,&nbsp;Amy Simon ,&nbsp;Ramanakumar Sankar","doi":"10.1016/j.icarus.2025.116868","DOIUrl":"10.1016/j.icarus.2025.116868","url":null,"abstract":"<div><div>We use spacecraft imaging and numerical modeling to analyze the morphology and dynamics of an interaction between a cyclone and an anticyclone in the northern hemisphere of Jupiter. The anticyclone, which is the smaller vortex, rotates around the cyclone such that it is displaced in latitude from one shear zone to the next. This is the first detailed characterization of an interaction of this type, showing an anticyclone crossing a cyclonic region. We also use a three-dimensional numerical model to identify and constrain vortex and environmental parameters that affect this behavior. Our results show that, depending on the initial latitudinal separation between the spots, their relative strength and the background static stability of the atmosphere, three distinct types of interactions that can occur. Namely, they can hop past each other, they can repel each other, or the cyclone can pull the anticyclone down as observed. The best match to the observed interaction and latitude displacement occurs for impact parameters less than <span><math><mrow><mo>≈</mo><mn>3</mn><msub><mrow><mi>L</mi></mrow><mrow><mi>d</mi></mrow></msub></mrow></math></span> and for values of the background static stability <span><math><mi>N</mi></math></span> between 8 and <span><math><mrow><mn>10</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>3</mn></mrow></msup><mspace></mspace><msup><mrow><mi>s</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span> at the bottom of the model, which would correspond to a high concentration of water in this region of the atmosphere, in which most of the lightning on the planet is detected.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116868"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145462554","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":"Micromechanical properties of Chang'e-5 lunar soil minerals: Comparison with meteorite and terrestrial analogs","authors":"Sijia Qiao ,&nbsp;Lihui Li ,&nbsp;Beixiu Huang ,&nbsp;Heng-Ci Tian","doi":"10.1016/j.icarus.2025.116872","DOIUrl":"10.1016/j.icarus.2025.116872","url":null,"abstract":"<div><div>The mechanical behavior of lunar materials holds significant engineering implications for lunar base construction and deep space exploration. However, the unique space weathering environment and complex regolith microstructure compromise the credibility of mechanical studies by terrestrial analogs, and the scarcity of returned lunar soil samples precludes repetitive macroscale laboratory testing. In this study, minimally destructive techniques—mineral identification and nanoindentation tests—were integrated to measure the microscale elastic modulus (<em>E</em>*) and hardness (<em>H</em>) of Chang'e-5 lunar soil (CE5‐054), lunar meteorite (NWA 4734), and terrestrial analog (CR-1). Results demonstrated notable variations in <em>E</em>* (87.1–173.2 GPa) and <em>H</em> (6.89–9.67 GPa) among CE5‐054 minerals, with olivine showing the highest <em>E</em>* and pyroxene showing the highest <em>H</em>. Differential mechanical responses were also observed for identical mineral group from different samples, where CE5‐054 exhibited intermediate values versus NWA 4734 and CR-1. These discrepancies probably stem from their weathering processes that lunar meteorite experienced more intense impacts than lunar soil, followed by terrestrial rock. This suggests that the significant influence of weathering processes on mechanical properties extends down to the microscale, inherently altering macroscale mechanical behavior. By characterizing the micromechanical properties of lunar soil, this study provides foundational data for lunar engineering design while advancing our understanding of mechanical property evolution through space weathering processes.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116872"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145462557","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 complete list of He-pressure-broadening coefficient of CO2 lines from 100 K to 3000 K for planet and exoplanet opacity calculations","authors":"Faten Hendaoui ,&nbsp;Jean-Michel Hartmann ,&nbsp;Hassen Aroui ,&nbsp;Ha Tran","doi":"10.1016/j.icarus.2025.116861","DOIUrl":"10.1016/j.icarus.2025.116861","url":null,"abstract":"<div><div>He pressure-broadening coefficients of CO₂ lines were predicted over a wide temperature range (100−3000 K) using requantized classical molecular dynamics simulations (rCMDS). This approach, based on the use of an ab initio intermolecular interaction potential, Newtonian equations of motion, and a requantized procedure, enables the calculation of the spectral density of He-broadened CO₂ spectra. The resulting spectra were fitted with the usual Voigt profile to deduce He-broadening coefficients. Requantization was calibrated to match the rCMDS-predicted broadenings coefficients to quantum scattering results at room temperature, available for thirteen lines, computed with the same potential. Comparisons between rCMDS and quantum calculations at 123 K and 760 K showed very good agreements. Excellent agreements with experimental data were also observed at 123 K, 160 K, 565 K, and 760 K. rCMDS calculations were then extended to several temperatures up to 3000 K, enabling prediction of broadening coefficients for rotational quantum numbers up to <em>J</em> = 240, where no prior theoretical or experimental data exist. The temperature dependence of the broadening coefficients was then modeled using either a double power-law model when applicable or the usual single power law. The resulting dataset provides He-broadening coefficients of CO₂ lines for <em>J</em> up to 166 for any temperature between 100 K and 3000 K. These results represent the most comprehensive set of line-shape parameters for CO₂ perturbed by He, providing improved input for spectroscopic databases and for opacity modeling in planetary and exoplanetary atmospheres.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116861"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145417806","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":"Earthquake detection in a simulated lunar regolith using distributed acoustic sensing","authors":"Amber Zandanel ,&nbsp;Kai Gao ,&nbsp;Simone Probst ,&nbsp;Johan O.A. Robertsson ,&nbsp;Carly M. Donahue","doi":"10.1016/j.icarus.2025.116848","DOIUrl":"10.1016/j.icarus.2025.116848","url":null,"abstract":"<div><div>Current models of inner lunar geology have largely been inferred from the seismic experiments and observations performed during the Apollo missions that comprised a relatively small number of seismic instruments. Refining constraints on fundamental lunar relationships such as crust-mantle and mantle-core boundaries in the future will require seismic arrays spanning larger epicentral distances. A promising technology for installing dense seismic arrays with minimal human effort is distributed acoustic sensing (DAS), an approach that allows a single length of fiber optic cable to act as hundreds or thousands of sensors when coupled with a DAS interrogator. While terrestrial uses of DAS technology for seismic monitoring rely on burying the cable to maximize fidelity of seismic signal transmission to the fiber, digging meters of trench to bury optical fiber on lunar or planetary surfaces is logistically infeasible. To evaluate DAS signal attenuation due to surface deployment of cable in lunar regolith, we completed earthquake detection analyses that evaluated the sensitivity of an optic-fiber DAS system to seismic signals at different burial depths. We deployed a single-mode fiber in a 10-m open-bottom wooden box filled with a lunar regolith simulant (LRS) with fiber buried at different depths within the LRS and recorded signals for four regional and local earthquakes. The results were used to identify and evaluate signal attenuation in surface-deployed fiber compared to buried fiber in the LRS. Burial depth responses to active-source signals were also evaluated similar to previous studies characterizing DAS sensitivity of surface-deployed fiber. Atmospheric noise was minimal as the cable was deployed in an indoor environment; however, where observed, atmospheric and anthropogenic noise was filtered out using the same bandpass filtering used to identify earthquake events. We found that signal attenuation of the surface-deployed fiber compared to buried fiber was relatively high in active-source experiments but was not consistently observed in earthquake signals. That burial depth is not highly correlated to attenuation of the observed earthquake signals indicates that in a noise-limited environment, placing DAS-interrogated fiber directly at the regolith surface may be a promising deployment strategy to consider for sensing remote seismic signals during lunar exploration.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116848"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145322269","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":"Characteristics and dynamics of spring-time northern cap-edge dust activities simulated by a Mars climate model","authors":"Z.H. Luo ,&nbsp;K.C. Chow ,&nbsp;J. Xiao","doi":"10.1016/j.icarus.2025.116843","DOIUrl":"10.1016/j.icarus.2025.116843","url":null,"abstract":"<div><div>Northern cap-edge dust storms during spring are major dust activities in the non-dusty season of Mars. In this study, we apply a parameterization scheme to the Mars climate model MarsWRF to simulate the dust activities in the northern cap-edge region. Consistent with observations, the simulation result shows a period of weak dust activities in the northern mid spring (Ls 30°-60°) and a stronger period just before the northern summer solstice, with a pause of dust activities between these two periods. The results of the sensitivity experiments suggest that the sublimation flow associated with cap recession is important to the occurrence of dust lifting but its effect on dust lifting near the cap edge could be different in different periods. The sublimation flow generally reduces the dust lifting flux in mid spring while enhances dust lifting at the end of spring. Three specific areas that are prone to dust lifting have also been identified. The simulation results suggest that the locations of the preferred dust lifting areas and the pause between the two active periods are possibly related to the topography in northern high latitudes.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116843"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145321757","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":"Orographic elongated clouds in mid-temperate and subpolar latitudes of Mars. I-Observations","authors":"E. Larsen ,&nbsp;A. Sánchez-Lavega ,&nbsp;T. del Río-Gaztelurrutia ,&nbsp;J. Hernández-Bernal","doi":"10.1016/j.icarus.2025.116864","DOIUrl":"10.1016/j.icarus.2025.116864","url":null,"abstract":"<div><div>We report new cases of extremely long and narrow clouds, visually similar in their morphology to the Arsia Mons elongated cloud (AMEC) (Hernández-Bernal et al., 2021a, 2022), that form at mid-temperate and subpolar latitudes in both hemispheres of the planet. We focus on four regions with different topography: the rugged mountain range of Thaumasia Highlands (267°E, 40°S), the volcanic region of Alba Patera (250°E, 40°N), the fretted and cratered highland terrain Tempe Terra (285°E, 48°N), and Lyot crater (29.3°E, 50.4°N). We use the images obtained by the Visual Monitoring Camera (VMC) on board the Mars Express mission, profiting from Mars Express' advantageous polar elliptical orbit, which allows us to characterize these clouds at different local times and spatial resolutions. At the elevated region of Thaumasia Highlands clouds form throughout the southern fall and winter during Ls = 0° – 170°, with lengths of up to 2700 km, widths of up to 220 km and heights 10–22 km above the surface. The elongated clouds at Alba Patera and Tempe Terra form during the northern fall and winter seasons between Ls = 180° – 330° with maximum lengths of 2600 km and 1900 km, maximum widths of 270 km and 240 km and heights between 10 and 27 km and 8–22 km respectively. Similarly, the elongated clouds at Lyot crater form during Ls = 180° – 340° and can have lengths of up to 2600 km and widths of up to 300 km. However, their heights are lower ranging 5–16 km over the surface.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116864"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145417805","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":"Formation conditions and chemical composition of early-condensed olivine in the solar protoplanetary disk","authors":"Elian Ochem,&nbsp;Yves Marrocchi","doi":"10.1016/j.icarus.2025.116859","DOIUrl":"10.1016/j.icarus.2025.116859","url":null,"abstract":"<div><div>The dynamic evolution of the solar protoplanetary disk led to the formation of the first solar system solids by condensation, among which amoeboid olivine aggregates (AOAs) are the most abundant. The conditions under which AOAs formed remain poorly constrained, with both equilibrium condensation under sub-solar dust/gas ratios and out-of-equilibrium condensation having been proposed. The recent identification of metal–olivine inclusions (MOIs) in carbonaceous chondrites (CCs) provides a unique opportunity to investigate the conditions of forsterite condensation. Our petrographic survey confirms the frequent occurrence of MOIs in CCs. Their occasional association with AOAs, together with the high MnO/FeO ratios and the ¹⁶O-rich composition of forsteritic rims, indicates formation by gas–solid condensation early in the disk's history. These forsteritic rims are chemically depleted in refractory elements such as Ca, Al, and Ti. Combined with existing literature data, our findings support the condensation of both AOAs and MOIs under out-of-equilibrium conditions during transient, localized heating events in a thermally heterogeneous and dynamically evolving disk. A comparison with relict olivine grains in type I chondrules suggests that AOA-MOI association represent plausible type I chondrule precursors. These results question models proposing that Ca–Al–Ti-rich refractory forsterite necessarily predates chondrule formation. Instead, we suggest that Ca–Al–Ti-poor olivine may better preserve information about the nature and conditions of early chondrule precursors.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116859"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145358790","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":"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":"2026-02-01","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":"Analytical estimates for heliocentric escape of satellite ejecta","authors":"Jose Daniel Castro-Cisneros ,&nbsp;Renu Malhotra ,&nbsp;Aaron J. Rosengren","doi":"10.1016/j.icarus.2025.116845","DOIUrl":"10.1016/j.icarus.2025.116845","url":null,"abstract":"<div><div>We present a general analytic framework to assess whether impact ejecta launched from the surface of a satellite can escape the gravitational influence of the planet–satellite system and enter heliocentric orbit. Using a patched-conic approach and defining the transition to planetocentric space via the Hill sphere or sphere of influence, we derive thresholds for escape in terms of the satellite-to-planet mass ratio and the ratio of the satellite’s orbital speed to its escape speed. We identify three dynamical regimes for ejecta based on residual speed and launch direction. We complement this analysis with the circular restricted three-body problem, deriving a necessary escape condition from the Jacobi integral at <span><math><msub><mrow><mi>L</mi></mrow><mrow><mn>2</mn></mrow></msub></math></span> and showing that it is consistent with the patched–conic thresholds. Applying our model to the Earth–Moon system reveals that all three outcomes — bound, conditional, and unbound — are accessible within a narrow range of launch speeds. This behavior is not found in other planetary satellite systems, but may occur in some binary asteroids. The framework also shows that the Moon’s tidal migration has not altered its propensity to produce escaping ejecta, reinforcing the plausibility of a lunar origin for some near-Earth asteroids.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116845"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145321773","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":"Late Amazonian-aged volcanic cones of explosive origin in Ceraunius Fossae, Tharsis, Mars","authors":"Bartosz Pieterek ,&nbsp;Thomas J. Jones ,&nbsp;Chiedozie C. Ogbuagu","doi":"10.1016/j.icarus.2025.116870","DOIUrl":"10.1016/j.icarus.2025.116870","url":null,"abstract":"<div><div>Detailed volcanological studies continue to enhance our understanding of Martian eruptive styles and their associated volcanic products. Growing evidence points to the involvement of mildly explosive eruptions as one of the eruption styles that contributed to the formation of distributed volcanic edifices in the volcanic province, Tharsis. This highlights a complex and dynamic eruptive evolution that occurred during the late Amazonian volcanism. Therefore, here, we report on the presence of small-scale, conical-shaped volcanic edifices located at the edge of Ceraunius Fossae in Tharsis. The association of the N-S aligned cones with a rough-surfaced lava flow enabled us to constrain the minimum age of their volcanic activity at ca. 48 Ma. Although they superficially resemble Martian scoria cones, their morphometric parameters indicate that they have a distinct and separate origin. They comprise coarser pyroclastic material such as spatter, and display an accumulation of likely volcanic bombs on the cones' slopes and at their bases, observable in the high-resolution images. Combining the sizes and distribution of the mapped individual volcanic bombs with a ballistic emplacement model enables us to calculate the exit velocity and maximum height for a given bomb density at a given launch angle. This provides a means to improve our understanding of ballistic trajectories and distances over which the pyroclastic material can be transported on Mars. Moreover, we argue that the portfolio of Martian volcanic edifices is more diverse than currently recognized. The use of high-resolution remotely sensed volcanological mapping could provide critical information about volcanic products and, consequently, the magma fragmentation, which depends on the eruptivity, controlled by magma composition and volatile contents.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116870"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145462683","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}