Planetary and Space Science最新文献

{"title":"Comparison of Kelvin–Helmholtz waves observed simultaneously at the dawn and dusk flanks of the Earth’s magnetopause","authors":"Niklas Grimmich ,&nbsp;Adriana Settino ,&nbsp;Heidi Katariina Nykyri ,&nbsp;Martin Owain Archer ,&nbsp;Kevin-Alexander Blasl ,&nbsp;Adrian Pöppelwerth ,&nbsp;Rumi Nakamura ,&nbsp;Ferdinand Plaschke","doi":"10.1016/j.pss.2025.106182","DOIUrl":"10.1016/j.pss.2025.106182","url":null,"abstract":"<div><div>Across the Earth’s magnetopause, unless the magnetic fields stabilise the boundary, the velocity shear between the magnetospheric plasma and the shocked plasma of the solar wind can lead to the Kelvin–Helmholtz instability. This instability can develop into large-scale surface waves and vortices at the magnetopause, causing the different plasma regions to mix, which plays an important role in the transfer of energy across the magnetopause. We know from spacecraft observations and simulations that the way Kelvin–Helmholtz waves grow and evolve can be different at dawn and dusk. However, very few studies have directly observed this phenomenon on both flanks of the magnetopause simultaneously, nor have they provided a consistent explanation for the question of symmetrical or asymmetrical dawn–dusk growth of the waves. By combining measurements from the THEMIS and Cluster missions, we can report here on an event where such a simultaneous observation of the Kelvin–Helmholtz waves is possible.</div><div>For this event, we investigate and compare the typical wave parameters and the plasma mixing on the two flanks. Our results suggest an asymmetric evolution of the Kelvin–Helmholtz waves at dawn and dusk. Comparing these results with previous studies of simultaneously observed events and linking them to solar wind conditions further shows that this asymmetric growth seems to occur during the Parker spiral IMF, but probably only if the magnetic fields are strong enough to effectively stabilise the boundary at the dusk flank due to field line draping.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"267 ","pages":"Article 106182"},"PeriodicalIF":1.7,"publicationDate":"2025-08-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144867090","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":"A generic compensation method for dynamic systematic errors in the geolocation of linear pushbroom satellite imagery","authors":"Da Li ,&nbsp;Yonghua Jiang ,&nbsp;Jingyin Wang ,&nbsp;Shaodong Wei ,&nbsp;Guo Zhang ,&nbsp;Huilong Wang","doi":"10.1016/j.pss.2025.106139","DOIUrl":"10.1016/j.pss.2025.106139","url":null,"abstract":"<div><div>In Earth observation and planetary exploration missions, high-precision geolocation through remote sensing is crucial. However, dynamic systematic errors in satellite imagery and ancillary flight data, arising from sensor limitation and measurement technology, challenge traditional correction methods such as orientation image model and bias compensation model. This study proposes a piecewise bias matrix compensation method to improve the geolocation accuracy of linear pushbroom cameras by effectively eliminating dynamic systematic errors. The method focuses on detect orientation point exposure time utilizing the distribution characteristics of the reprojection residuals caused by dynamic system errors. This is accomplished through a stepwise strategy involving residual point cloud thinning and iterative end-point fitting algorithms, which automatically divide the sub-compensation model. Furthermore, considering the stability of the satellite’s flight attitude, a Lagrange interpolation method is introduced in the piecewise bias matrix compensation model, enhancing the internal consistency and absolute accuracy in the geometric positioning process of the optical linear pushbroom satellite. A comparison of the initial camera positioning results in the experimental dataset revealed that the reprojected errors of conjugate points in the MEX-HRSC can now achieve sub-pixel accuracy, with a maximum root mean square error of 0.54 pixels; the reprojected errors of GCPs in the XX-18 can now achieve sub-pixel accuracy, with a maximum root mean square error of 0.80 pixels. Additionally, building upon the elimination of dynamic systematic errors, this study constructs high spatial resolution DTMs of the Martian surface using high-resolution stereo imagery from the MEX-HRSC. These techniques and methods result in the intersection of corresponding rays in stereo pairs, which is crucial for subsequent 3D reconstruction.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"267 ","pages":"Article 106139"},"PeriodicalIF":1.7,"publicationDate":"2025-08-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144842496","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":"Comet 12P/Pons-Brooks: Dust properties","authors":"R.S. Garcia ,&nbsp;E. Fernández-Lajús ,&nbsp;R.P. Di Sisto ,&nbsp;R.A. Gil-Hutton","doi":"10.1016/j.pss.2025.106181","DOIUrl":"10.1016/j.pss.2025.106181","url":null,"abstract":"<div><div>Comet 12P/Pons-Brooks, a Halley-type comet with a 71-year orbital period, was first discovered in 1812. It follows a highly inclined trajectory, originating from just beyond Neptune’s orbit. Ground-based observations have shown that the comet exhibited activity at a heliocentric distance of 11 au during its approach to the Sun. Numerous studies have since focused on its behavior, particularly its pre-perihelion outbursts, which have provided valuable insights into its dynamic and volatile nature.</div><div>This study examines the dust behavior of 12P following its perihelion passage. Using the 0.6 m Helen Sawyer Hogg telescope at the Complejo Astronómico El Leoncito (CASLEO), a series of images were captured between May and June 2024 using broadband I, R, and V filters. Morphological, photometric, and numerical analyses were performed to investigate the comet’s dust characteristics. Enhanced imaging revealed two active regions within an isotropic coma, which contributed to its distinctive “devil comet” appearance. Photometric analysis, based on the magnitudes and dust production rate from the <span><math><mrow><mi>A</mi><mrow><mo>(</mo><mn>0</mn><mo>°</mo><mo>)</mo></mrow><mi>f</mi><mi>ρ</mi></mrow></math></span> parameter, indicated ordinary dust behavior, with no characteristic outbursts observed.</div><div>To gain further insights into 12P’s dust behavior, the data were fitted to a new theoretical model for studying dust in comets. This model suggests that the dust coma primarily consisted of large particles emitted from two high-latitude active areas at a velocity of approximately <span><math><mrow><mn>409</mn><mspace></mspace><msup><mrow><mtext>ms</mtext></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span>, assuming a rotation period of 57 h.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"267 ","pages":"Article 106181"},"PeriodicalIF":1.7,"publicationDate":"2025-08-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144867091","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 the directional nature of the fall of celestial objects on the surface of Venus","authors":"Debashis Chatterjee ,&nbsp;Prithwish Ghosh","doi":"10.1016/j.pss.2025.106167","DOIUrl":"10.1016/j.pss.2025.106167","url":null,"abstract":"<div><div>This study demonstrates the critical need for circular data analysis in interpreting meteor impact locations on Venus. Traditional linear methods need to be improved to capture the cyclic nature of these data. We can better identify patterns and trends using specialized circular data techniques, enhancing our understanding of the mechanisms behind meteor impacts. By employing specialized statistical techniques that capture the cyclic nature of angular data, our analysis included Watson’s test at a 0.05 significance level, showing that the Venus surface crater dataset’s location parameters and solar elevations conform to a Von Mises distribution, while daytime and nighttime solar elevations do not. Using Bayesian Information Criterion (BIC) scores, we also determine that a two-component mixture of Fisher–von Mises distributions best models the spatial distribution of impact craters. These findings enhance our understanding of meteor impact processes on Venus and highlight the advantages of applying maximum-entropy directional models to planetary science.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"266 ","pages":"Article 106167"},"PeriodicalIF":1.7,"publicationDate":"2025-07-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144767142","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":"A shocked lithic clast with compositionally contrasting melt domains in the impact melt breccia-a first report from the Dhala impact structure, India","authors":"Jayanta Kumar Pati ,&nbsp;Anuj Kumar Singh ,&nbsp;Shivanshu Dwivedi","doi":"10.1016/j.pss.2025.106180","DOIUrl":"10.1016/j.pss.2025.106180","url":null,"abstract":"<div><div>Bolide impacts are associated with enormous amount of kinetic energy which transforms into humongous shock pressures (∼100 GPa) and temperatures (up to 20,000 °C) on the planetary surfaces. These extreme conditions result in unique shock features that are routinely used as diagnostic evidence to confirm the meteorite impact origin of a structure. Occurrence of diaplectic glass pseudomorphing various minerals is one of the unequivocal evidences of shock metamorphism. Similarly, complete rock melting requires pressure in the excess of 60 GPa; however, the melting processes are not well constrained and remain ambiguous. The present study focuses on shock-induced melting of a quartzo-feldspathic lithic clast within an impact melt breccia sample from the Dhala structure, India. Multiple felsic melt stringers and a silicic melt (similar to lechatelierite) lense were observed across the clast, displaying a linear mixing trend between K-feldspar and silica. The occurrences of planar deformation features in quartz, melt clasts, spherules, and traces of coesite indicate characteristics of shock metamorphism. The presence of coesite (a high-pressure silica polymorph), formed during shock pressure release from the silica melt, was verified through Raman spectroscopy. Compositions of felsic melt stringers seem to mimic eutectic melting similar to a synthetic K₂O-Al₂O₃-SiO₂ system suggesting the dominant role of eutectic type punctuated melting rather than instantaneous melt behaviour. This pattern contrasts with an immediate, widespread melting often reported in impactites worldwide.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"266 ","pages":"Article 106180"},"PeriodicalIF":1.7,"publicationDate":"2025-07-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144771267","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":"Water-group ion irradiation studies of Enceladus ice analogues: Can radiolysis account for material in and around the south polar plume?","authors":"Grace Richards ,&nbsp;Richárd Rácz ,&nbsp;Sándor T.S. Kovács ,&nbsp;Victoria Pearson ,&nbsp;Geraint Morgan ,&nbsp;Manish R. Patel ,&nbsp;Simon Sheridan ,&nbsp;Duncan V. Mifsud ,&nbsp;Béla Sulik ,&nbsp;Sándor Biri ,&nbsp;Nigel J. Mason ,&nbsp;Robert W. McCullough ,&nbsp;Zoltán Juhász","doi":"10.1016/j.pss.2025.106179","DOIUrl":"10.1016/j.pss.2025.106179","url":null,"abstract":"<div><div>Saturn's magnetosphere contains trapped plasma and energetic charged particles which constantly irradiate the surface of Enceladus. In this study, we exposed Enceladean surface ice analogues containing H₂O, CO₂, CH₄, and NH₃ to water-group ions (e.g., O⁺, O³⁺, OH⁺, and H₂O⁺) having energies between 10 and 45 keV with the aim of exploring the chemical evolution of these ices and characterising the extent to which the surface material on Enceladus is weathered by Saturn's radiation environment. Each irradiation process was monitored <em>in situ</em> using Fourier-transform mid-infrared transmission absorption spectroscopy, and post-irradiative warming of the ices was performed to better characterise complex organic molecules formed as a result of the mobilisation of radiolytically generated radicals. Irradiation resulted in the formation of CO, OCN⁻, and NH₄⁺ in all experiments, and the radiolytic formation of formamide, acetylene, acetaldehyde, and hydroxymethyl radicals was also tentatively suggested in most experiments. Post-irradiative warming of the ices resulted in the formation of carbamic acid, ammonium carbamate, and an alcohol species. Although many of these products have not been previously observed on Enceladus' surface, some have been detected in Enceladus' plumes. Since our results demonstrate that the radiolytic formation of these molecules can occur over timescales similar to the exposure times of plume and surface material to magnetospheric radiation, questions must be raised as to whether such material originates directly from the subsurface ocean or is instead formed within the radiation-rich space environment.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"266 ","pages":"Article 106179"},"PeriodicalIF":1.7,"publicationDate":"2025-07-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144722323","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 the formation of satellites in dense solid-particle disks","authors":"G. Madeira ,&nbsp;L. Esteves ,&nbsp;T.F.L.L. Pinheiro ,&nbsp;P.V.S. Soares ,&nbsp;N.S. Santos ,&nbsp;B. Morgado","doi":"10.1016/j.pss.2025.106168","DOIUrl":"10.1016/j.pss.2025.106168","url":null,"abstract":"<div><div>Single massive satellites are of great observational interest, as they can produce prominent and potentially detectable signatures. For terrestrial planets and super-Earths, giant impacts in the late stages of formation may generate dense self-gravitating disks — favourable environments for the formation of such satellites. Motivated by this, we explore satellite formation in dense solid-particle disks through three-dimensional N-body simulations, focusing on the effects of disk mass and the surface density exponent (<span><math><mi>β</mi></math></span>). Our results reveal significant variability in the masses and configurations of satellites formed under identical disk parameters, highlighting the stochastic nature of the process. Higher disk masses and flatter surface density profiles favour the formation of more massive satellites. Disks with masses above 0.03 planetary masses typically yield a single dominant satellite, while those between 0.003 and 0.03 tend to form two-satellite systems. On average, the mass of the largest satellite scales linearly with the initial disk mass, in agreement with analytical predictions. We estimate that a disk with a minimal mass of 0.03 planetary masses around a 1.6 Earth-mass planet orbiting a Sun-like star could form an Earth–Moon-like system detectable by telescopes with a photometric precision of 10 parts per million – a level achievable by the James Webb Space Telescope.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"266 ","pages":"Article 106168"},"PeriodicalIF":1.8,"publicationDate":"2025-07-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144665815","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":"Experimental investigation of solar radiation effects on Mercury’s surface regolith","authors":"Nicole Latsia ,&nbsp;Georgios Tsirvoulis ,&nbsp;Erika Kaufmann ,&nbsp;David Haack ,&nbsp;Mikael Granvik ,&nbsp;Axel Hagermann","doi":"10.1016/j.pss.2025.106166","DOIUrl":"10.1016/j.pss.2025.106166","url":null,"abstract":"<div><div>The surface of Mercury is exposed to extreme diurnal thermal variations caused by the high intensity of solar radiation, the radiative loss due to the planet’s lack of atmosphere, its eccentricity and its 3:2 spin - orbit resonance. This work presents an experimental study on terrestrial rocks used as Mercury analogues subjected to hermean conditions. We simulate the power density of a planetary surface at Mercury’s perihelion distance of 0.31 au using the Space and High-Irradiance Near-Sun Simulator (SHINeS) at Luleå University of Technology. The reflectance spectra were acquired in the visible and near-infrared wavelength range for every sample before and after irradiation. Permanent spectral changes are observed in all samples towards the longer wavelengths in the visible spectrum after only one thermal cycle. Darkening is evident in both the visible and near-infrared spectrum ranges, combined with reddening in the visible-to-near-infrared region in most of our samples. We propose that darker samples like boninite, basalt, and diorite are more likely to experience spectral changes due to their low albedo.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"266 ","pages":"Article 106166"},"PeriodicalIF":1.8,"publicationDate":"2025-07-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144663289","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":"Thermal and electrochemical properties of a mixture of lunar regolith simulant (FJS-1) and CaF2","authors":"Yuta Suzuki ,&nbsp;Seiya Tanaka ,&nbsp;Takuya Goto","doi":"10.1016/j.pss.2025.106177","DOIUrl":"10.1016/j.pss.2025.106177","url":null,"abstract":"<div><div>To establish the electrochemical reduction process of lunar regolith as an in-situ resource utilization technology on the Moon, it is crucial to prepare a high-temperature electrolytic melt that has a composition suitable for electrolysis. In this study, we propose a mixed melt consisting of lunar regolith, which comprises metal-oxide compounds, and CaF₂, which can be collected from fluorapatite on the Moon's surface. To characterize the lunar regolith-CaF₂ system, the thermal and electrochemical properties of a mixture of a lunar mare regolith simulant (FJS-1) and CaF₂ were investigated. The differential thermal analysis curves measured for various compositions of FJS-1 and CaF₂ found that the eutectic temperature was 1275 K at FJS-1:CaF₂ = 90:10 wt%, which is lower than the melting point of FJS-1, 1393 K. By electrochemical impedance spectroscopic technique, the electrical resistance of the melts at 1673 K was found to be 43 Ω for the FJS-1 melt, while the mixed melt of FJS-1 and CaF₂ (80:20 wt%) was found to be 5 Ω. The XRD analysis of the solidified melts revealed that the mixed melts' unique physical properties were due to the formation of chemical bonding of F⁻ ions due to CaF₂ and metal ions due to FJS-1. Furthermore, the electrochemical behavior of the mixed melt was investigated, demonstrating the electrodeposition of metals such as Si and Al derived from FJS-1. The reported data will provide new guidelines for designing electrolytic systems on the Moon, expanding the possibilities for controlling the temperature and electrochemical operations.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"266 ","pages":"Article 106177"},"PeriodicalIF":1.8,"publicationDate":"2025-07-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144656459","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":"A composite phase function for cometary dust comae","authors":"Ivano Bertini ,&nbsp;Jean–Baptiste Vincent ,&nbsp;Raphael Marschall ,&nbsp;Fiorangela La Forgia ,&nbsp;Alessandra Mura ,&nbsp;Laura Inno ,&nbsp;Stavro Ivanovski ,&nbsp;Michael Küppers ,&nbsp;Cecilia Tubiana ,&nbsp;Vladimir Zakharov","doi":"10.1016/j.pss.2025.106164","DOIUrl":"10.1016/j.pss.2025.106164","url":null,"abstract":"<div><div>Comets represent the most preserved planetesimals we can nowadays study and dust is one of their major components. Once emitted in the coma, cometary dust particles represent anisotropic scatterers of the incident solar light and their nature can be investigated with remote sensing studies. Among them, the measurement of the phase function curve has a key importance in several scientific aspects. It can be inverted with theoretical and laboratory studies to derive hints on the intimate nature of the emitted dust. It is also needed in adjusting cometary dust production rates for phase angle effects when data obtained throughout large time intervals are correlated. Finally, it is useful for space instruments planning since it provides inputs for optimal exposure times for remote sensing sensors which observe the coma spanning a large range of phase angles during close approaches. This will be particularly valuable in the framework of the future ESA Comet Interceptor mission which is going to fly-by a Dynamically New Comet entering our Inner Solar System for the very first time, carrying instruments which will image the coma with different observing geometries and phase angles in a short amount of time. In order to provide an useful tool to address the aforementioned scientific topics, we used available literature data to build a new composite phase function for cometary dust comae. This was obtained fitting Henyey–Greenstein functions to the original data of 11 comets and then connecting them in a continuous way as all data values were coming from a single average comet. We then fitted our result with a compound Henyey–Greenstein curve and compared it with previous models which were not including recent literature data constituting fine follow-ups of comets at small and large phase angles. The main difference is found in the description of the forward scattering surge, where our model depicts intensity one order of magnitude larger than previous ones. This finding is extremely important since it shows that the choice of the model may have severe consequences when interpreting, or instrumentally planning, forward scattering data.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"265 ","pages":"Article 106164"},"PeriodicalIF":1.8,"publicationDate":"2025-07-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144580289","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}