Icarus最新文献

{"title":"Long-distance ranging and velocity measurements by REASON on Europa Clipper","authors":"Michelle S. Park ,&nbsp;Gregor Steinbrügge ,&nbsp;Elizabeth Wig ,&nbsp;Dustin M. Schroeder ,&nbsp;Erwan Mazarico ,&nbsp;Donald D. Blankenship","doi":"10.1016/j.icarus.2025.116585","DOIUrl":"10.1016/j.icarus.2025.116585","url":null,"abstract":"<div><div>One of the objectives of the Gravity and Radio Science (G/RS) instrument on NASA’s Europa Clipper mission is to improve our knowledge of Europa’s ephemerides, to trace the moon’s thermal-orbital evolution. Here, we present a complementary methodology to use the Radar for Europa Assessment and Sounding: Ocean to Near-surface (REASON) instrument to enhance these measurements by tracking echoes from Europa at greater distances, beyond its primary role of subsurface sounding during close flybys. We investigate the possibility of occasional REASON measurements during the non-nadir phase at altitudes beyond 40,000 km to extend the ephemerides dataset. Through radar simulations of REASON’s echoes, we evaluate and demonstrate this approach by determining the maximum altitude for surface return detection, achieved by coherently processing hundreds to thousands of pulses within the signal’s round-trip time. The received signal’s power can be further enhanced by maximizing pulse length, targeting Europa’s most reflective (leading sub-Jovian) hemisphere, and summing many compressed pulses. We also explore a phase shift approach for velocity measurements, which uses existing ranging pulses. Using Europa Clipper’s most recent trajectory design, we identify flybys that align with the best working scenarios for this approach. Our performance estimates for range and velocity resolution demonstrate that this approach could obtain measurements relevant to Europa’s ephemerides. This method offers key insights into Europa’s orbital evolution and, ultimately, its long-term habitability.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116585"},"PeriodicalIF":2.5,"publicationDate":"2025-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143834830","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":"Climatology of transient eddies and dust storms in the southern hemisphere of Mars","authors":"David Hinson","doi":"10.1016/j.icarus.2025.116581","DOIUrl":"10.1016/j.icarus.2025.116581","url":null,"abstract":"<div><div>This paper examines the behavior of transient eddies in the southern hemisphere of Mars and illustrates how the eddies shape the annual cycle and spatial distribution of dust storms. The investigation of transient eddies is based on off-nadir measurements of brightness temperature by the Mars Climate Sounder, which are the most direct and reliable source of information about eddy activity adjacent to the surface. Basic properties of the transient eddies are determined through least-squares analysis of brightness temperatures spanning 8.6 Mars years, yielding a far more complete description of eddy activity in the southern hemisphere than was available previously. The space-time spectrum is dominated by eddies with zonal wavenumbers 1–4 and periods shorter than 5 sols. The wave-4 component is much more important than was previously recognized. An annual cycle comprising three distinct periods of eddy activity is observed each year. Shallow (in temperature) baroclinic waves are present at <span><math><mrow><msub><mrow><mi>L</mi></mrow><mrow><mi>s</mi></mrow></msub><mo>=</mo><mn>0</mn></mrow></math></span>–<span><math><mrow><mn>75</mn><mo>°</mo></mrow></math></span> and <span><math><mrow><mn>125</mn></mrow></math></span>–<span><math><mrow><mn>200</mn><mo>°</mo></mrow></math></span>. In the intervening period, the baroclinic waves are replaced by a deep, 3.3-sol, barotropic wave that has a relatively small amplitude near the surface. The transient eddies strongly influence the annual cycle of discrete dust storms cataloged in the Mars Dust Activity Database and the Mars Dust Storm Sequence Dataset. Dust storms are rare and their net area is negligible during the barotropic phase of eddy activity (<span><math><mrow><msub><mrow><mi>L</mi></mrow><mrow><mi>s</mi></mrow></msub><mo>=</mo><mn>75</mn></mrow></math></span>–<span><math><mrow><mn>125</mn><mo>°</mo></mrow></math></span>), when the amplitude near the surface is small. Conversely, the wind stress routinely exceeds the threshold required for dust lifting during the two baroclinic phases of eddy activity, when the amplitude near the surface is much larger, resulting in a conspicuous increase in the net area of the dust storms. Dust storms occur frequently in a corridor extending from Aonia Terra to Margaritifer Terra, owing to the presence of a persistent storm track of eddy activity in the western hemisphere. The density of dust storms in this corridor varies in response to the seasonal evolution in the strength and latitude of the storm track. Further insight is gained by consolidating results from previous studies. This investigation improves our understanding of the Martian climate in the half year centered on the southern winter solstice, when the atmosphere is relatively cool and clear.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116581"},"PeriodicalIF":2.5,"publicationDate":"2025-04-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143807942","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":"Effects of observation geometry and heating on the ultra-violet to near-infrared spectra of Mercury simulant","authors":"Mireia Leon-Dasi ,&nbsp;Sebastien Besse ,&nbsp;Camille Cartier ,&nbsp;Océane Barraud ,&nbsp;Alessandro Maturilli ,&nbsp;Alain Doressoundiram ,&nbsp;Johannes Benkhoff ,&nbsp;Laurie Llado","doi":"10.1016/j.icarus.2025.116582","DOIUrl":"10.1016/j.icarus.2025.116582","url":null,"abstract":"<div><div>The temperature of Mercury varies greatly across different latitudes due to the planet’s spin/orbit resonance, leading to modifications in the surface spectral properties. The upcoming BepiColombo mission will map the surface of the planet in the UV-TIR range, providing a more comprehensive understanding of the surface alteration. However, comparing the spectral measurements between BepiColombo and the past MESSENGER mission could be challenging due to the large differences in observation geometry. Laboratory experiments with close surface analogs in viewing conditions similar to the space-based observations are necessary to understand the effect of the space environment and interpret the orbital spectral measurements. This study presents the UV-NIR spectroscopy of a Mercury simulant to understand the impact of observation geometry and temperature on the spectral properties of the planet’s surface. The simulant (a mixture of aubrites, albite, and synthetic sulfides) and its endmembers are measured under six geometries that sample the viewing conditions of both missions. The samples are measured fresh and after heating to 450 °C during three cycles. This study finds that the observation geometry modifies the reflectance spectrum of the samples differently depending on the wavelength and composition. The analog presents a darkening, reddening, and flattening with increasing phase angle in the UV-NIR domain. The heated samples present a brightening and reddening, with a deepening of absorption bands. The spectral changes associated with observation geometry and heating are stronger with increasing Mg abundance.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116582"},"PeriodicalIF":2.5,"publicationDate":"2025-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143807943","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":"Modelling the effect of volcanic outgassing of sulphur on early Martian surface temperatures using a 3-D Global Climate Model","authors":"A.S. Braude ,&nbsp;L. Kerber ,&nbsp;F. Lefèvre ,&nbsp;A.Y. Jaziri ,&nbsp;S.S. Hamid ,&nbsp;M. Lefèvre ,&nbsp;M. Maurice ,&nbsp;E. Millour ,&nbsp;F. Forget","doi":"10.1016/j.icarus.2025.116568","DOIUrl":"10.1016/j.icarus.2025.116568","url":null,"abstract":"<div><div>Around the time of the transition from the Late Noachian to the Early Hesperian eras (<span><math><mo>∼</mo></math></span>3.6 Gya), Mars was predicted to have been both volcanically active, and have sustained a climate warm enough to melt liquid water on its surface episodically despite a faint young sun. The effect of volcanic outgassing on the climate of early Mars and its ability to raise temperatures above the melting point of water has, however, been disputed, with a major uncertainty being the timescales over which the greenhouse effect of outgassed sulphur dioxide (SO₂) and hydrogen sulphide (H₂S) can warm the atmosphere of Mars before they react to form H₂SO₄ and S₈ aerosols which act to cool the surface of Mars. We have developed the first 3-D model of the Martian sulphur cycle from source to sink that includes outgassing of SO₂, H₂S and S₂ from the surface, the formation of H₂SO₄ and S₈ through atmospheric chemistry, and the condensation and deposition of H₂SO₄ and S₈ to the surface. We simulate the effect of a single large, day-long volcanic outgassing event on global surface temperatures, identifying the magnitude and duration of any net warming and cooling as a function of outgassing magnitude, atmospheric pressure, obliquity and aerosol particle size distribution. We confirm the results of Tian et al. (2010, EPSL 295, 412-418) and find that the persistence of the warming effect of volcanically outgassed SO₂ and H₂S on the Martian atmosphere is only of the order of days to weeks for a surface pressure range of between 0.5 and 1.5 bars. Typical outgassing magnitudes result in a net cooling of the Martian surface over timescales of 3–4 years near the equator and several decades at the poles for plume neutral buoyancy heights within the troposphere. For very high magnitudes of outgassing, the rate of H₂SO₄ cloud formation slows down due to the depletion of water vapour in the atmosphere, thereby slowing down the rate of cooling and providing a buffer against atmospheric collapse.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116568"},"PeriodicalIF":2.5,"publicationDate":"2025-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143820569","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":"Investigating grain size in the Martian mantle: Implications of basal mantle layers and viscoelastic models","authors":"Feng Liang ,&nbsp;Jianguo Yan ,&nbsp;Chi Xiao ,&nbsp;Yuji Harada ,&nbsp;Jean-Pierre Barriot","doi":"10.1016/j.icarus.2025.116592","DOIUrl":"10.1016/j.icarus.2025.116592","url":null,"abstract":"<div><div>This study examines the grain size in the Martian mantle using viscoelastic dissipation models and two interior structural configurations: S23M1 (without a basal mantle layer, BML) and S23M2 (with a BML). Results indicate substantial variations in grain size estimates depending on the viscoelastic model employed. For instance, Andrade(<em>μ-β</em>) models suggest smaller grain sizes (∼1 mm), while Burgers(background), Burgers(+peak), and Andrade(fixed <em>β</em>) models predict a broader range of 0.1–10 cm. Sundberg-Cooper models, by contrast, yield larger grain sizes (&gt;0.5 cm). The inclusion of a BML generally leads to smaller grain size estimates. For instance, Sundberg-Cooper predictions decrease from ∼10 cm to ∼0.8 cm with a BML, attributed to altered average rigidity of Mars that reduces elastic response. These findings stress the importance of mantle structure in interpreting viscoelastic properties and reconciling laboratory-derived constraints with geophysical observations. Future tidal measurements are critical for refining these models further.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116592"},"PeriodicalIF":2.5,"publicationDate":"2025-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143834829","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":"An energy-angular momentum phase function for rubble pile asteroids","authors":"D.J. Scheeres","doi":"10.1016/j.icarus.2025.116563","DOIUrl":"10.1016/j.icarus.2025.116563","url":null,"abstract":"<div><div>This work analyzes the energetics of asteroid rubble piles in order to understand what asteroid morphologies should naturally arise from their formation and evolution process. In doing this, a phase diagram is developed that maps out the range of final minimum energy states that a collapsing gravitational aggregate can achieve as a function of total angular momentum and mass distribution. This is developed assuming properties associated with rubble pile asteroids, and can provide insight into the formation and subsequent evolution of contact binaries and orbital binaries in the solar system as an outcome of catastrophic disruptions. The system angular momentum is used as an independent parameter, combined with resulting minimum energy configurations as a simple function of mass morphology of the final system. The configuration of systems with an energy boosted above the minimum energy state are also considered. This paper considers an ideal case, but outlines general results that can be continued for more precise models of distributed granular media modeled using continuum models or using discrete element models.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116563"},"PeriodicalIF":2.5,"publicationDate":"2025-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143786107","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 source of hydrogen in earth's building blocks","authors":"Thomas J. Barrett ,&nbsp;James F.J. Bryson ,&nbsp;Kalotina Geraki","doi":"10.1016/j.icarus.2025.116588","DOIUrl":"10.1016/j.icarus.2025.116588","url":null,"abstract":"<div><div>Despite being pivotal to the habitability of our planet, the process by which Earth gained its present-day hydrogen budget is unclear. Due to their isotopic similarity to terrestrial rocks across a range of elements, the meteorite group that is thought to best represent Earth's building blocks is the enstatite chondrites (ECs). Because of ECs' nominally anhydrous mineralogy, these building blocks have long been presumed to have supplied negligible hydrogen to the proto-Earth. However, recent bulk compositional measurements suggest that ECs may unexpectedly contain enough hydrogen to readily explain Earth's present-day water abundance. Together, these contradictory findings mean the contribution of ECs to Earth's hydrogen budget is currently unclear. As such, it is uncertain whether appreciable hydrogen is a systematic outcome of Earth's formation. Here, we explore the amount of hydrogen in ECs as well as the phase that may carry this element using sulfur X-ray absorption near edge structure (S-XANES) spectroscopy. We find that hydrogen bonded to sulfur is prevalent throughout the meteorite, with fine matrix containing on average almost 10 times more H<img>S than chondrule mesostasis. Moreover, the concentration of the H<img>S bond is linked to the abundance of micrometre-scale pyrrhotite (Fe_1-xS, 0 &lt; x &lt; 0.125). This sulfide can sacrificially catalyse a reaction with H₂ from the disk at high temperatures to create H₂S, which could be dissolved in adjoining molten silicate-rich material. Upon rapid cooling, this assemblage would form pyrrhotite encased in submicron silicate-rich glass that carries trapped H₂S. These findings indicate that hydrogen is present in ECs in higher concentrations than previously considered and could suggest that this element may have a systematic, rather than stochastic, origin on our planet.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116588"},"PeriodicalIF":2.5,"publicationDate":"2025-04-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143864671","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":"Asteroid phase curves and phase coloring effect using the ATLAS survey data","authors":"Milagros Colazo ,&nbsp;Dagmara Oszkiewicz ,&nbsp;Alvaro Alvarez-Candal ,&nbsp;Patrycja Poźniak ,&nbsp;Przemysław Bartczak ,&nbsp;Edyta Podlewska-Gaca","doi":"10.1016/j.icarus.2025.116577","DOIUrl":"10.1016/j.icarus.2025.116577","url":null,"abstract":"<div><div>We determined phase curves for 301<span><math><mo>,</mo></math></span>272 asteroids in the orange filter and 280<span><math><mo>,</mo></math></span>953 in the cyan filter from the latest ATLAS Solar System Catalog V2 (SSCAT-2). Among them, 3<span><math><mo>,</mo></math></span>345 and 492 asteroids in the orange and cyan filters, respectively, have uncertainties below 15%. Our simple model, which considers only the apparition effect, showed good consistency with more sophisticated methods requiring much less computational time. Database cross-matching allowed us to analyze G1 and G2 distributions according to taxonomy. We conducted two-dimensional Kolmogorov–Smirnov tests to investigate two distinct aspects: similarities in paired G1, G2 distributions across different taxa and wavelength dependency within the same taxa. When comparing different taxa, we could not reject the null hypothesis for 11% of the orange sample and 31% of the cyan sample, indicating more disparities in the orange filter. For wavelength dependency, paired distributions of G1, G2 (o) vs. G1, G2 (c) showed statistically significant differences across all complexes, except for the A class. Our analysis suggests that while phase coloring behaviors are observed without a clear preference for reddening or bluening at phase angles below 5°, reddening predominates in the 10°–30°range. We also observed smaller uncertainties in G2 than in G1. Simulations showed that G2 is less sensitive to lack of data at small phase angles. This is related to the definition of the H, G1, G2 function, where G1 contributes more to the opposition effect and G2 the linear part of the phase curve. Our catalog-independent algorithms are adaptable to new data sets, including future LSST data.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116577"},"PeriodicalIF":2.5,"publicationDate":"2025-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143799738","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":"Correction for calcium interference in the 40Ar/39Ar dating method","authors":"Wan-Feng Zhang ,&nbsp;Jun-Jie Wang ,&nbsp;De-Wen Zheng ,&nbsp;Ming Xiao ,&nbsp;Jia Zhang ,&nbsp;Jun-Jie Li ,&nbsp;Yu-Lian Zhang ,&nbsp;Ying-De Jiang ,&nbsp;Fei Su ,&nbsp;Li Li ,&nbsp;Yi-Gang Xu","doi":"10.1016/j.icarus.2025.116591","DOIUrl":"10.1016/j.icarus.2025.116591","url":null,"abstract":"<div><div>Since the inception of the ⁴⁰Ar/³⁹Ar dating method, it has been recognized that fast neutrons can interact with nuclides in the sample beyond ³⁹K, resulting in the production of interfering argon isotopes. Correction factors for these side effects have been proposed from many nuclear reactors globally. However, current practice does not always involve the monitoring of these correction factors for every sample batch, but is reliant on previous results instead. This approach is justified by the limited variability observed in the (³⁶Ar/³⁷Ar)_Ca and (³⁹Ar/³⁷Ar)_Ca correction factors, and such limited variability is acceptable for samples with high K/Ca ratio. For low K/Ca samples, however, even minor variations in the correction factors can significantly impact the accuracy of the results. Here, we evaluate the performance of optical grade CaF₂ crystals and spectrally pure-grade CaF₂ to monitor the correction factor for the calcium interference. The results demonstrate that the optical grade CaF₂ crystals yield consistently reliable calcium correction factors when subjected to stepwise heating and single grain total fusion. Therefore, we recommend the use of optical grade CaF₂ crystals for monitoring potential calcium interference. Furthermore, we advocate for the continuous monitoring of calcium correction factors during each sample irradiation. When analyzing extraterrestrial samples, the optical grade CaF₂ crystals should be positioned adjacent to the samples. As a standard product, optical grade CaF₂ crystals are readily accessible to ⁴⁰Ar/³⁹Ar laboratories worldwide.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"435 ","pages":"Article 116591"},"PeriodicalIF":2.5,"publicationDate":"2025-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143776366","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":"Analysis on the source position of Zhinyu crater ejecta","authors":"Huacheng Li ,&nbsp;Zongyu Yue ,&nbsp;Nan Zhang","doi":"10.1016/j.icarus.2025.116579","DOIUrl":"10.1016/j.icarus.2025.116579","url":null,"abstract":"<div><div>Impact craters are prevalent features on the Moon, and a significant volume of materials from the impact site is delivered to distant during their formation. The impact ejecta is closely related with many other surface processes, and some empirical equations inherent have been proposed in the studies. For example, a power-law relationship indicating a decrease in ejecta thickness with distance has been derived from dimensionless analysis, and it has been verified through laboratory experiments, numerical simulations, and remote sensing observations. A power-law relationship between launch speed and position of ejected materials is also suggested. However, no simple power-law exists for the initial and maximum excavation depths and the final position of ejecta. In this study, we used high-resolution numerical simulations of Zhinyu crater to explore the relationship between excavation depth and ejecta distance. A model for maximum excavation depth, based on the Maxwell <em>Z</em>-model, was further presented and found consistent with numerical simulation results.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"435 ","pages":"Article 116579"},"PeriodicalIF":2.5,"publicationDate":"2025-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143767474","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}