Journal of Geophysical Research: Space Physics最新文献

{"title":"Geoeffectivity of Solar Wind Heavy Ions","authors":"Chris Jia, Susan T. Lepri, Liang Zhao, Jim M. Raines, Daniel Welling, Jennifer A. Carter, Simona Nitti","doi":"10.1029/2025JA034257","DOIUrl":"https://doi.org/10.1029/2025JA034257","url":null,"abstract":"<p>The influence of solar wind properties, such as the southward interplanetary magnetic field, on geomagnetic activity has been well established. However, the role of heavy ions (i.e., particles heavier than protons) in the solar wind on geomagnetic storms is not fully understood. Notably, scientific models and simulations of the Earth's magnetosphere predominately assume a pure-proton solar wind, despite heavy ions constituting over 15% of the solar wind mass density on average during solar maximum periods. By utilizing data from Solar Wind Ion Composition Spectrometer onboard the Advanced Composition Explorer (ACE), we investigate the impact of heavy ion dynamic pressure during Interplanetary Coronal Mass Ejection (ICME) events on Earth's magnetosphere. Including heavy ion dynamic pressure into magnetopause calculations leads to an average reduction of 3.25% in Earth's magnetopause standoff distance during the ICME sheath interval, which could be larger during specific events. Additionally, we observe that heavy ions yield stronger correlations between maximum ion dynamic pressures during ICMEs and the corresponding minimum <i>Dst</i> and maximum auroral electrojet (AE) indices. The correlations with minimum <i>Dst</i> and maximum <i>AE</i> are stronger when considering minor ions (i.e., heavy ions excluding helium), with correlation coefficients of <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mrow>\u0000 <mi>r</mi>\u0000 <mo>=</mo>\u0000 <mo>−</mo>\u0000 <mn>0.57</mn>\u0000 </mrow>\u0000 </mrow>\u0000 <annotation> $r=-0.57$</annotation>\u0000 </semantics></math> and <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mrow>\u0000 <mi>r</mi>\u0000 <mo>=</mo>\u0000 <mn>0.60</mn>\u0000 </mrow>\u0000 </mrow>\u0000 <annotation> $r=0.60$</annotation>\u0000 </semantics></math>, respectively, compared to <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mrow>\u0000 <mi>r</mi>\u0000 <mo>=</mo>\u0000 <mo>−</mo>\u0000 <mn>0.48</mn>\u0000 </mrow>\u0000 </mrow>\u0000 <annotation> $r=-0.48$</annotation>\u0000 </semantics></math> and <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mrow>\u0000 <mi>r</mi>\u0000 <mo>=</mo>\u0000 <mn>0.43</mn>\u0000 </mrow>\u0000 </mrow>\u0000 <annotation> $r=0.43$</annotation>\u0000 </semantics></math> for protons alone. These findings underscore the importance of including heavy ions in solar wind models to improv","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA034257","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272435","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":"Propagation of Whistler-Mode Waves in a Combination of Density and Magnetic Field-Aligned Irregularities","authors":"Anatoly V. Streltsov","doi":"10.1029/2025JA034527","DOIUrl":"https://doi.org/10.1029/2025JA034527","url":null,"abstract":"<p>The paper presents results from the analytical and numerical investigations of the propagation of whistler-mode waves in the magnetosphere containing field-aligned irregularities of the plasma density and the magnetic field. Whistler-mode waves can be guided along the field by the field-aligned irregularities consisting of the enhancement or depletion of the plasma density (high-density or low-density ducts). It also can be guided by the irregularities consisting of the enhancement or depletion of the magnetic field (high-magnetic or low-magnetic ducts). We demonstrate that these density and magnetic ducts considered together can “enhance” or “degrade” ducting of the whistler-mode waves by each other. Specifically, the low-density duct enhances wave trapping by the high-magnetic duct and degrades the wave trapping by the low-magnetic duct and vice versa. The high-density duct enhances wave trapping by the low-magnetic duct and degrades the wave trapping by the high-magnetic duct and vice versa.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272254","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":"Statistical Study of Wave Properties of Power Line Harmonic Radiation at the Fundamental Frequency and Its Third Harmonic in the Topside Ionosphere","authors":"Zhuangkai Wang,&nbsp;Xiang Xu,&nbsp;Chen Zhou","doi":"10.1029/2025JA034187","DOIUrl":"https://doi.org/10.1029/2025JA034187","url":null,"abstract":"<p>The wave properties of the power line harmonic radiation (PLHR) at the fundamental frequency 60 Hz and its third harmonic 180 Hz in the topside ionosphere are investigated statistically using the magnetic field data of China Seismo-Electromagnetic Satellite in the year of 2023. The spatial distributions of the wave properties including the polar angle, the azimuthal angle, and the polarization are obtained from the automatically identified events and their dependence on various factors are analyzed based on the statistical results. We find that the polar angles of PLHR at 60 Hz are generally larger at low magnetic latitudes (|MLAT| &lt; 30°) than that at higher magnetic latitudes (|MLAT| &gt; 30°). The large polar angles at high magnetic latitudes away from the high-occurrence region may be associated with the wave reflection of PLHR at 60/180 Hz. The wide longitudinal distribution of PLHR at 60/180 Hz with low occurrence rates outside of the high-occurrence region meridian planes may be explained by the azimuthal propagation of PLHR indicated by the large variation of the azimuthal angles. The latitudinal, diurnal and monthly variations of the polarization of PLHR at 60/180 Hz may be associated with the altitude of the local crossover frequency surface dependent on the ambient ion fraction and geomagnetic field strength. The occurrence rates of the left-handedly polarized PLHR are significantly higher at 180 Hz than that at 60 Hz, which may be due to the lower altitude of the crossover frequency surface at 180 Hz.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272255","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":"Investigation of the Diffusion Region With Varying Turbulence Intensities Around the X-Line of Magnetotail Reconnection","authors":"Xinmin Li,&nbsp;Rongsheng Wang,&nbsp;Chuanfei Dong,&nbsp;Quanming Lu,&nbsp;San Lu,&nbsp;Julia E. Stawarz,&nbsp;Yi Qi,&nbsp;Liang Wang,&nbsp;J. L. Burch","doi":"10.1029/2025JA034426","DOIUrl":"https://doi.org/10.1029/2025JA034426","url":null,"abstract":"<p>Magnetic reconnection and turbulence are two fundamental processes in space plasma environments. They are intricately coupled, driving energy transfer and conversion. Despite significant research efforts, the development of turbulence within the reconnection diffusion region and its impact on the reconnection process remain open questions. In this study, we analyze 16 magnetotail reconnection cases observed by the Magnetospheric Multiscale (MMS) mission, focusing on the diffusion regions in the vicinity of the X-line. We find that turbulence tends to be stronger in diffusion regions with lower plasma density and plasma beta. Turbulence can enhance the electron energization process in the diffusion region primarily through electron heating. As turbulence intensifies, the continuous current layer of the diffusion region breaks into fragmented currents, suggesting a transition from laminar to turbulent reconnection. Moreover, spectral breaks between ion and electron cyclotron frequencies are consistently observed in magnetic and electric field fluctuations within reconnecting current sheets, suggesting that such breaks may be a characteristic feature of the reconnection process. These findings provide valuable insights into the development and role of turbulence within the reconnection diffusion region.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272555","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":"Electron Thermal Flux and Temperature Maps Based on the Global Survey of Electron Precipitation Due To Whistler-Mode Waves","authors":"George V. Khazanov,&nbsp;Qianli Ma,&nbsp;Mike Chu","doi":"10.1029/2025JA034453","DOIUrl":"https://doi.org/10.1029/2025JA034453","url":null,"abstract":"<p>Electron thermal fluxes entering upper ionospheric altitudes define electron temperature distribution down to the F ionospheric layer. Electron heat/thermal fluxes are formed at magnetospheric altitudes by many different heating mechanisms via interactions of plasmaspheric cold background electrons with hot magnetospheric population and wave-particle interaction processes. However, the knowledge of electron precipitation distribution driven by the waves on the global scale is limited and requires additional experimental, data analysis, and theoretical studies. This paper uses a comprehensive global survey of electron precipitation and whistler waves by Ma et al. (2020, 2021, https://doi.org/10.1029/2020gl088798, https://doi.org/10.1029/2021ja029644) that based on Van Allen Probes observations from September 2012 to September 2019. The electron precipitation and whistler waves were used as an input to SuperThermal ElecTrons transport code to reveal the role of magnetosphere-ionosphere-atmosphere energy interplay the formation of electron heat fluxes entering upper ionospheric altitudes. The electron heat fluxes and temperature results that are presented in this manuscript cover the AE index ranges of AE &lt; 100 nT, 100 &lt; AE &lt; 500 nT, and AE &gt; 500 nT, as the function of geographical and magnetic latitudes and magnetic local time, and are only affiliated with whistler wave activities.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272025","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":"Relativistic Electron Flux Oscillations in the Earth's Outer Radiation Belt: A Statistical Study","authors":"Xinxin Chu,&nbsp;Chaoling Tang,&nbsp;Zhenpeng Su,&nbsp;Jingrun Chen","doi":"10.1029/2025JA034359","DOIUrl":"https://doi.org/10.1029/2025JA034359","url":null,"abstract":"<p>Using the data from the Van Allen Probes, we statistically studied 2.1 MeV electron flux oscillation events in the Earth's outer radiation belt during non-storm activities. Based on the different magnetic local times (MLT), the oscillation events are divided into “dayside events” (DE, 6 ≤ MLT ≤ 18) and “nightside events” (NE, 18 &lt; MLT &lt; 6). These NEs are divided into “weak substorm events” (WSE, <i>AE</i> &lt; 200 nT) and “strong substorm events” (SSE, <i>AE</i> &gt; 200 nT). The SSE is further divided into “strong substorm with low solar wind dynamic pressure change (Δ<i>P</i>_sw) events” (SSLP, <i>AE</i> &gt; 200 nT, Δ<i>P</i>_sw &lt; 5 nPa) and “strong substorm with high Δ<i>P</i>_sw events” (SSHP, <i>AE</i> &gt; 200 nT, Δ<i>P</i>_sw &gt; 5 nPa). Our statistical results show that: (a) For DE, WSE, and SSHP, Δ<i>P</i>_sw and solar wind speed (<i>V</i>_sw) are the main factors affecting the oscillation location, while Δ<i>P</i>_sw is the dominant factor affecting the oscillation amplitude. The interplanetary magnetic field <i>B</i>_z component has no significant effects on the oscillations of DE. These results support the idea that these oscillations are mainly caused by ultralow frequency (ULF) waves excited by Δ<i>P</i>_sw; (b) For SSLP, substorm activity and <i>V</i>_sw do not affect the oscillation location. However, the intense substorm activity and Δ<i>P</i>_sw can cause a large oscillation amplitude. This shows the idea that these oscillations are mainly caused by a combination of ULF waves excited by Δ<i>P</i>_sw and substorm activity. These can help us further understand the ULF waves and relativistic electron dynamics of the Earth's outer radiation belt.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272064","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":"Evidence for a Natural Limit to Electron Space Radiation: An Application of Benford's Law","authors":"L. Olifer,&nbsp;I. R. Mann","doi":"10.1029/2025JA034445","DOIUrl":"https://doi.org/10.1029/2025JA034445","url":null,"abstract":"<p>Recent research has highlighted observational evidence for a natural limit to the severity of energetic electron differential fluxes in the Van Allen radiation belts. Here, we analyze the occurrence distributions of electron differential fluxes from the entire Van Allen Probes mission (2012–2019) to further investigate the energy dependence of electron flux distributions under the action of the flux-capping mechanism proposed by Kennel and Petschek (1966, https://doi.org/10.1029/jz071i001p00001). Specifically, we further examine the characteristics of the ensemble of flux values for at least weak geomagnetic activity (Dst<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>&lt;</mo>\u0000 <mo>−</mo>\u0000 </mrow>\u0000 <annotation> ${&lt; } -$</annotation>\u0000 </semantics></math>30 nT) in the context of Benford's Law. Benford's Law proposes a logarithmic distribution of the first significant digit of ensembles of numerical values of various parameters, and has been found to be obeyed across a wide range of scientific, socioeconomic, and even financial data sets. We show that Benford's Law can be used to distinguish between the energies of electron flux distributions that are either strongly affected or largely unaffected by flux-capping Kennel-Petschek-like processes. In this paper, we present a representative numerical model of ensemble distributions formed through a large number of sequential multiplicative operations (such as those expected from repeated wave-particle interactions in the Van Allen belts). The model demonstrates that in the absence of capping processes, these distributions naturally evolve into log-normal forms. Furthermore, their first-digit occurrence distributions closely follow Benford's Law.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA034445","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272613","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":"Steepened Ultra-Low Frequency Waves and Foreshock Dynamics in the Upstream Martian Bow Shock Region","authors":"Gangkai Poh,&nbsp;Jared Espley,&nbsp;Shaosui Xu,&nbsp;Norberto Romanelli,&nbsp;Jacob Gruesbeck,&nbsp;Guan Le,&nbsp;Jasper Halekas,&nbsp;Gina DiBraccio","doi":"10.1029/2025JA033708","DOIUrl":"https://doi.org/10.1029/2025JA033708","url":null,"abstract":"<p>We presented the analysis of steepened ultra-low frequency (ULF) waves in the region upstream of Mars' bow shock observed by the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft. We surveyed MAVEN measurements for magnetic fields and plasma signatures associated with compressive steepened waves, mainly (a) large-amplitude, quasi-periodic gradual increase followed by sharp decrease in |<b>B</b>| (i.e., shock-like) with corresponding complex rotations in the measured magnetic field, (b) enhanced proton and electron fluxes at energies greater than that of the solar wind, and (c) occasional observation of discrete, quasi-monochromatic higher frequency wave packets at the leading edges of the steepened waves. We identified 16 intervals when MAVEN observed steepened waves, and from these 16 wave intervals, we identified 79 individual steepened wave events (or wave cycles) over 1.5 years of MAVEN data. Our statistical analysis indicates that these steepened waves occur at an average frequency (in the spacecraft frame) of ∼0.5 local proton gyrofrequency (Ω_<i>i</i>), magnetic compression ratio of ∼3.52 and time separation of ∼48 s. Statistical analysis also indicates no obvious preference in the spatial occurrence of these steepened waves, with most events observed near the boundary between quasi-parallel and perpendicular shock regions; there is also no obvious correlation between their spatial occurrence and solar wind conditions (e.g., <i>P</i>_dyn and <i>M</i>_A). Our results support the idea proposed by earlier studies that the steepened wave events presented in this study are likely to be steepened from the ULF waves associated with the photo-ionization of the proton in the extended martian hydrogen corona.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272614","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":"Automated Bow Shock Identification and Multi-Spacecraft Timing Using Magnetospheric Multiscale (MMS) Observations","authors":"Vicki Toy-Edens,&nbsp;Savvas Raptis,&nbsp;Drew L. Turner,&nbsp;Wenli Mo,&nbsp;Sean A. Q. Young","doi":"10.1029/2025JA034252","DOIUrl":"https://doi.org/10.1029/2025JA034252","url":null,"abstract":"<p>Utilizing 8 years of dayside Magnetospheric Multiscale (MMS) mission plasma region identifications, we present an automatically identified and manually verified data set of 2,594 bow shock crossings in MMS burst-mode. For each bow shock crossing, we identify the bow shock ramp in each MMS probe using two automated methods and apply multi-spacecraft timing to calculate the bow shock normal. The bow shock list was separated into quasi-parallel and quasi-perpendicular based on the presence or absence of ion foreshock in order to evaluate deviations between the automated methods and a statistical 3D bow shock model. There are large discrepancies between global and local shock properties where the local shock properties are highly skewed towards quasi-perpendicular properties regardless of the presence of ion foreshock. Although this skewness grows when the tetrahedral configuration is suboptimal, it persists even under ideal formation, indicating that electron-scale processes can modulate local shock properties. These findings highlight the limitations of local multi-spacecraft timing in accurately characterizing shock geometry without contextual information, such as the presence of an upstream foreshock or a similarly disturbed downstream magnetosheath. Ultimately, this data article provides thousands of high-resolution bow shock crossings for further scientific research by the community.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA034252","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272091","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":"Ducting Propagation of Whistler Waves Inside Magnetic Peaks: Considering Hot Electron Effects","authors":"Xiongdong Yu,&nbsp;Zhigang Yuan,&nbsp;Fei Yao,&nbsp;Zuxiang Xue,&nbsp;Dan Deng","doi":"10.1029/2025JA034625","DOIUrl":"https://doi.org/10.1029/2025JA034625","url":null,"abstract":"<p>Recent studies have demonstrated that whistler-mode waves in the terrestrial magnetosphere can be trapped inside a magnetic peak under the cold plasma approximation. However, the effect of hot electrons on the ducting propagation of whistler waves by the magnetic peak remains uncovered yet. Here, using kinetic theory to include the contribution of hot electrons, we have shown that magnetic peaks could still prompt a ducting effect on the propagation of whistler waves, even when hot electrons dominate. Moreover, we performed a parameter analysis and found that for a higher fractional density of hot electrons or electrons with a higher temperature, a larger refractive index is required for whistler waves to be trapped. These theoretical results have been verified with an observational event of the Van Allen Probe mission, suggesting the necessity to consider hot electrons, especially when discussing the propagation of whistler waves in magnetic peaks outside the plasmasphere.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272615","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}