Journal of Geophysical Research: Space Physics最新文献

{"title":"Control of Solar Wind on Magnetic Field Fluctuations in the Subsolar Magnetosheath","authors":"Ying Zou,&nbsp;Brian M. Walsh,&nbsp;Yuxi Chen,&nbsp;Hongyang Zhou,&nbsp;Savvas Raptis","doi":"10.1029/2025JA033856","DOIUrl":"https://doi.org/10.1029/2025JA033856","url":null,"abstract":"<p>The magnetosheath modifies the solar wind and IMF before they reach Earth's magnetosphere, and hence plays a crucial role in regulating the solar wind-magnetosphere interaction. Although the steady component of the magnetosheath magnetic field has been reasonably well reproduced, the fluctuating component has been less accounted for despite its significant amplitude. This paper empirically determines the mean characteristics of the ultra-low-frequency magnetic field fluctuations, and constructs a functional form using solar wind parameters. We use 15 years of THEMIS A data for the magnetosheath, and OMNI for the upstream solar wind conditions. Qualitatively, fluctuations are negatively correlated with the IMF cone angle, and positively with the solar wind speed and dynamic pressure. Some fluctuations are correlated with the IMF strength but not all. The level of fluctuations in the IMF is positively correlated with &lt;0.01 Hz fluctuations in the magnetosheath. A higher Mach number is associated with a larger fraction of compressional versus transverse fluctuations in the magnetosheath. Quantitatively, the correlation between magnetosheath fluctuations and individual solar wind parameters is weak, correlation magnitude being &lt;0.5. However, by performing a multiple linear regression fit of the solar wind parameters to magnetosheath fluctuations, a reasonably good prediction can be achieved with correlation magnitude in the range of 0.5–0.7, except for the parallel magnetosheath fluctuations of 0.01–0.1 Hz. Our results are overall consistent with earlier studies, but our quantitative approach further permits forecast of how much the IMF changes inside the magnetosheath which is beneficial for scientific understanding and space weather forecasts.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 6","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-06-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144264655","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Occurrence Variability of Severe Scintillation and Range Spread F From the Varying Nature of Large-to-Meso-Scale-Wave-Structures: Observations and Simulation","authors":"B. C. Amadi,&nbsp;E. A. Kherani,&nbsp;E. R. de Paula","doi":"10.1029/2025JA033840","DOIUrl":"https://doi.org/10.1029/2025JA033840","url":null,"abstract":"<p>The occurrence variability on a day-to-day basis of severe S4 scintillation and range-spread F (RSF) which are the manifestations of the most robust dynamical spread F phenomenon in the nighttime equatorial-low-latitude ionosphere, remains intriguing to date. The complex nature of large-to-meso-scale-wave-structure (LSWS) that results from the two most important determining factors, large-scale pre-reversal electric field (PREF) and Meso-Scale wave electric field, poses a severe obstacle to the short-term forecasting of S4-RSF. The present study aims to investigate the competing role of the two factors by presenting S4-RSF events that occur during the summer months of 2021–2022 over the Equatorial region of Brazil. The scintillation index (S4) and total-electron-content (TEC) from the GNSS network and ionospheric drift measurements from digisonde found more frequent occurrences of severe S4-RSF during December 2021 than in January 2022. The measurements detect LSWS in both months, though December reveals phase propagation of TEC and drift oscillations for longer horizontal distances and altitudes. The strength variability of S4-RSF is understood by conducting the numerical simulation of collisional-interchange instability. In line with the observations, the simulation shows the stronger and faster equatorial plasma bubble formations from the combined action of PREF and phase-coherent mesoscale electric field. Despite the comparatively weak PREF, the stronger S4-RSF activities highlight the role of mesoscale wave electric field in defining the strength of S4-RSF.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 6","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-06-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA033840","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144264656","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Magnetosheath Jets Associated With a Solar Wind Rotational Discontinuity in a Hybrid-Vlasov Simulation","authors":"Jonas Suni,&nbsp;Minna Palmroth,&nbsp;Lucile Turc,&nbsp;Markus Battarbee,&nbsp;Yann Pfau-Kempf,&nbsp;Urs Ganse","doi":"10.1029/2025JA033995","DOIUrl":"https://doi.org/10.1029/2025JA033995","url":null,"abstract":"<p>Magnetosheath jets are transient enhancements of dynamic pressure downstream of collisionless shocks. In Earth's magnetosheath they are mostly found downstream of the quasi-parallel bow shock during steady solar wind and low interplanetary magnetic field (IMF) cone angle conditions, but they have also been observed in the quasi-perpendicular magnetosheath and during different solar wind conditions. In this study we use a 2D simulation run of the global hybrid-Vlasov model Vlasiator to investigate how the interaction between the bow shock and a solar wind rotational discontinuity influences the formation of magnetosheath jets. Separating the jets identified in the simulation based on formation site and time relative to the interaction between the discontinuity and the shock, we conduct a statistical study to find the characteristic properties of the different jet types. We find that jets forming at the quasi-parallel shock are similar to each other regardless of the stage of the shock-discontinuity interaction. Jets forming at the quasi-perpendicular shock after the discontinuity has passed are small and short-lived. The jets forming at the quasi-perpendicular shock as the discontinuity impacts it, on the other hand, merge with each other into a large and long-lived transient density enhancement that propagates deep into the magnetosheath together with the discontinuity, giving it the potential to be more geoeffective than the other types. This study sheds light on the properties of jets and jet-like structures that form during non-steady solar wind and IMF conditions, and the results can be of use when classifying similar events from spacecraft observations.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 6","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-06-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA033995","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144244884","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Spatio-Temporal Evolution of Mid-Latitude GPS Scintillation and Position Errors During the May 2024 Solar Storm","authors":"Waqar Younas,&nbsp;Yukitoshi Nishimura,&nbsp;Weixuan Liao,&nbsp;Josh L. Semeter,&nbsp;Sebastijan Mrak,&nbsp;Y. Jade Morton,&nbsp;Keith M. Groves","doi":"10.1029/2025JA033839","DOIUrl":"https://doi.org/10.1029/2025JA033839","url":null,"abstract":"<p>This study investigates impacts of the May 2024 superstorm on the mid-latitude Global Positioning System (GPS) scintillation and position errors. Using 1-Hz GPS receiver data, we identified position errors in PPP mode reaching up to 70 m in the Central United States during the storm main phase on May 10. The PPK solution becomes unstable following the arrival of storm and lasted till the recovery phase, coinciding with reported GPS outages of farming equipment. The large position errors were attributed to strong scintillation and carrier phase cycle slips around the equatorward boundary of the ionosphere trough, where large total electron content (TEC) gradients and irregularities were present. In the Southwestern United States, position errors of 10–20 m were associated with the storm-enhanced density and equatorial ionization anomaly. Scintillation and cycle slips in this region were minor, and bending of the GPS signal paths (refractive effect) is suggested to cause the position errors. PPP outages were also associated with sudden changes in the geometric distributions of available GPS satellites used in position calculations. On May 11, energetic particle precipitation during substorms led to abrupt jumps in TEC and scintillation, resulting in rapidly evolving position errors of up to 10 m. These findings highlight the critical role of storm-time plasma transport, precipitation, and irregularity formation in degrading GPS performance. The study underscores the need for accurate ionospheric state specification, improved signal processing technique, real-time ionospheric corrections, and optimized satellite selection algorithms, to enhance navigation resilience during severe space weather events.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 6","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-06-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144244954","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Particle-In-Cell Simulations of Starfish Prime","authors":"Mikhail A. Belyaev,&nbsp;David J. Larson,&nbsp;Bruce I. Cohen","doi":"10.1029/2024JA033681","DOIUrl":"https://doi.org/10.1029/2024JA033681","url":null,"abstract":"<p>The Starfish Prime high altitude nuclear test created a transient diamagnetic cavity in the Earth's magnetic field above Johnston Island and launched an electromagnetic pulse (EMP) that was detected around the globe. We use the ion-kinetic particle-in-cell code Topanga to simulate diamagnetic cavity evolution and the E3 EMP signal for Starfish Prime out to over a minute of physical time. The simulation domain has a longitudinal and latitudinal extent of <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mn>60</mn>\u0000 <mo>°</mo>\u0000 <mo>×</mo>\u0000 <mn>60</mn>\u0000 <mo>°</mo>\u0000 </mrow>\u0000 <annotation> $60{}^{circ}times 60{}^{circ}$</annotation>\u0000 </semantics></math> and a vertical extent of 2,000 km from the surface of the Earth. We compare our simulated results to magnetometer measurements taken in space and on the ground, finding good agreement in both cases. The diamagnetic cavity in the simulation forms in about a second, while the associated debris flux tube takes approximately 30 s to decay. The debris flux tube undergoes significant motion during this timeframe, rising upward. The measured E3 EMP signal on the ground consists of several components, all of which are present in our simulations. We discuss the physical origin of these components in relation to E3a (blast) and E3b (heave).</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 6","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-06-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144244169","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Effects of Solar Flares on the Ionosphere of Mars: Comparison of Observed and Predicted Electron Density Profiles From 15 to 26 April 2001","authors":"Paul Withers,&nbsp;A. G. Cramer,&nbsp;D. J. Pawlowski","doi":"10.1029/2024JA033197","DOIUrl":"https://doi.org/10.1029/2024JA033197","url":null,"abstract":"<p>Solar flares significantly affect Mars's ionosphere, yet there are few comparisons between observed and simulated densities in the M1 and M2 ionospheric layers during solar flares. Here we compare observed and simulated electron density profiles for the X14.4 solar flare of 15 April 2001 and the M7.8 solar flare of 26 April 2001. We use observations from Mars Global Surveyor radio occultations and simulations from the Mars Global Ionosphere-Thermosphere Model (M-GITM). Due to poor constraints on the solar spectrum incident upon Mars at this time, simulated M2 electron density values were 50% larger than observed. Yet the relative changes in M2 electron density during these two flares were reproduced to 10% accuracy. When accurate solar irradiance data are available, absolute M2 electron density values are simulated accurately. Due to the omission of electron impact ionization from the M-GITM model, the simulated M1/M2 density ratio was under-predicted by a factor of approximately 3. Yet the relative changes in M1 electron density during these two flares were reproduced to 20% accuracy. The model can accurately predict relative changes in M1 and M2 electron densities during a solar flare. If accurate solar irradiance data are available, it can accurately predict absolute changes in M2 electron densities. If a simple parameterization of electron impact ionization were incorporated into the model, then it would likely predict absolute changes in M1 electron densities accurately as well. The M-GITM model is well-suited to studies of time-varying phenomena in the ionosphere of Mars.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 6","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-06-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144220346","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Radio Wave Polarization of Saturn Lightning Observed by Cassini","authors":"G. Fischer,&nbsp;M. Imai,&nbsp;U. Taubenschuss,&nbsp;D. Píša,&nbsp;W. S. Kurth","doi":"10.1029/2024JA033560","DOIUrl":"https://doi.org/10.1029/2024JA033560","url":null,"abstract":"<p>We investigate the polarization of the radio waves emitted by lightning in Saturn's atmosphere, which are referred to as SEDs for Saturn Electrostatic Discharges. Using the complete SED data set retrieved by Cassini's RPWS (Radio and Plasma Wave Science) instrument we found that the circular polarization of SEDs below a frequency of 2 MHz depends on the latitudinal hemisphere of the lightning storm. SEDs from several storms located at <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mn>35</mn>\u0000 <mo>°</mo>\u0000 </mrow>\u0000 <annotation> $35{}^{circ}$</annotation>\u0000 </semantics></math> South latitude display a strong right–hand sense of circular polarization, whereas SEDs from storms located at <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mn>35</mn>\u0000 <mo>°</mo>\u0000 </mrow>\u0000 <annotation> $35{}^{circ}$</annotation>\u0000 </semantics></math> and <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mn>50</mn>\u0000 <mo>°</mo>\u0000 </mrow>\u0000 <annotation> $50{}^{circ}$</annotation>\u0000 </semantics></math> North are overwhelmingly left–hand polarized. A single storm located at Saturn's equator in June 2005 shows 4 right–handed SEDs when Cassini was in the northern hemisphere and 4 left–handed SEDs when Cassini was in the southern hemisphere. The polarization characteristic is consistent with an emission in the L-O mode, consistent with the theory of Fischer, Gurnett, et al. (2007, JGR 112, A12308, https://doi.org/10.1029/2007JA012592) that the R-X mode is largely absorbed in Saturn's ionosphere below a frequency of 2 MHz. The sense of circular SED polarization below 2 MHz is opposite to the polarization of Saturn kilometric radiation (SKR), and thus this can be used to distinguish SEDs from SKR and to determine the hemispherical origin of the causative lightning storm.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 6","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-06-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JA033560","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144220345","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Substorm Event Retrieval Model in Ultraviolet Aurora Images Based on Contextual CNN Features","authors":"Ze-Jun Hu,&nbsp;Bing Han,&nbsp;Bairu Zhao,&nbsp;Yang Lu,&nbsp;Yi-Sheng Zhang,&nbsp;Bei-Chen Zhang","doi":"10.1029/2025JA033983","DOIUrl":"https://doi.org/10.1029/2025JA033983","url":null,"abstract":"<p>Auroral substorms are one of the disturbance phenomena caused by high-energy charged particles from the solar wind precipitating into the Earth's magnetosphere and colliding with charged particles within the magnetosphere. Understanding the occurrence and evolution of substorms can help elucidate the physical processes governing the interaction between the solar wind and Earth's magnetosphere. Currently, ground-based and satellite-based imaging equipment have captured a vast amount of aurora images, and identifying auroral substorm events from these images is crucial for studying solar-terrestrial relations. The westward traveling surge (WTS) is a typical structure during substorm occurrences and is commonly used for auroral substorm identification. In this paper, we propose a method based on convolutional neural networks (CNNs) that uses a polar region partitioning strategy to locate image keypoints and determine the position and size of regional blocks. Multi-scale contextual CNN features are then generated to retrieve substorm events from ultraviolet aurora images. The results show that the multi-scale features extracted from convolutional and fully connected layers can effectively capture the characteristics of the WTS structure. The method achieves a mean average precision of 75.77% and a Recall@10 of 95.19%, demonstrating its effectiveness in retrieving auroral substorm events.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 6","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-06-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144213753","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Species-Dependent and Azimuthally-Directional Flux Changes of Dispersionless Ion Injections Inside Geosynchronous Orbit","authors":"T. Motoba,&nbsp;S. Ohtani","doi":"10.1029/2025JA033757","DOIUrl":"https://doi.org/10.1029/2025JA033757","url":null,"abstract":"<p>Dispersionless injection, involving sudden, simultaneous flux enhancements of energetic particles over a broad range of energy, is a characteristic signature of the particles that are experiencing a significant acceleration and/or rapid inward transport process. To provide clues to the physical processes that lead to the acceleration and transport of energetic ions in the dispersionless injection region, we conduct superposed epoch analyses of 75 dispersionless injection events identified by Van Allen Probes with focus on the species- and azimuthal angle- (<i>φ</i>) dependent signatures of ∼50–600 keV ions inside geosynchronous orbit. Our analysis shows that, on average, the light (hydrogen and helium) ion fluxes undergo a rapid, transient enhancement, while the heavy (oxygen) ion fluxes exhibit a more gradual, persisting enhancement. Such a species-dependent behavior could be explained in terms of different gyro-radius of the ion species. For events where the proton injection onset is 30–60 s earlier than the electron one, proton fluxes initially increase at small <i>φ</i> values (i.e., tailward guiding centers) and then at larger <i>φ</i> values (earthward ones). The initial signatures suggest a result of the earthward transport of injected protons, as seen at the explosive growth phase. For events where both electron and proton fluxes increase simultaneously, on the other hand, proton fluxes isotropically increase with no significant <i>φ</i> dependence. Such an isotropic proton flux enhancement may imply a local process in which charged protons are rapidly accelerated to higher energies at the spacecraft location.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 6","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-06-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA033757","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144214189","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Periodic Density Structures Around the Plasmaspheric Plume Boundary and Their Association With ULF Waves","authors":"Ting-Yan Xiang,&nbsp;Jie Ren,&nbsp;Qiu-Gang Zong,&nbsp;Zi-Jian Feng,&nbsp;Xin-Yu Ai","doi":"10.1029/2025JA034044","DOIUrl":"https://doi.org/10.1029/2025JA034044","url":null,"abstract":"<p>Here we report that the dynamics of the plasmaspheric plume can be affected by ULF waves based on observations from Van Allen Probes. Probe A observed periodic density structures with regular waveforms when traveling into the plume from its western boundary on 19 August 2013. The crests of the density structures were filled with intense hiss waves and low-energy <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mi>H</mi>\u0000 <mo>+</mo>\u0000 </msup>\u0000 </mrow>\u0000 <annotation> ${mathrm{H}}^{+}$</annotation>\u0000 </semantics></math> that also appeared in the plume. The in-phase relationship between toroidal magnetic field perturbations and density structures in the northern hemisphere indicates that the plume boundary was stretched westward when the field lines were moving westward. These observations indicate that periodic density structures stem from the azimuthal oscillations of the plume boundary under the drive of the fundamental toroidal mode of ULF waves. ULF waves around the plume boundary exhibit the largest amplitude and out-of-phase polarization, and the polarization is changing with MLT across the plume boundary, demonstrating that field line resonance (FLR) occurred at the plume boundary. These observations are consistent with the theoretically predicted characteristics of 3-D FLR associated with the plamspheric plume.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 6","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-06-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144213788","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}