Journal of Geophysical Research: Space Physics最新文献

{"title":"Study of Double-Pulse Magnetic Structure During Decoupling Expansion of Debris Plasma","authors":"Ziming Wang,&nbsp;Ye Dong,&nbsp;Mengmeng Song,&nbsp;Zhaohui Liu,&nbsp;Wei Yang,&nbsp;Qiang Sun,&nbsp;Wenbin Wu,&nbsp;Zhekai Luo,&nbsp;Hantian Zhang,&nbsp;Qianhong Zhou","doi":"10.1029/2024JA033641","DOIUrl":"https://doi.org/10.1029/2024JA033641","url":null,"abstract":"<p>The decoupling expansion of debris plasma refers to the process where debris plasma generated by a high-altitude nuclear explosion (HANE) slips through the ambient plasma. Unlike the coupled expansion of the debris plasma and ambient plasma, decoupling expansion leads to a smaller magnetic cavity and wider debris dispersal. This significantly alters the magnetic field structures within hundreds of kilometers around the HANE center and even the artificial radiation belt at higher altitude. In this paper, the evolution mechanism of the double-pulse magnetic structure is investigated by simulating the decoupling expansion process of super- Alfvénic debris plasma using a two-dimensional hybrid model. It is found that the rapidly formed azimuthal electron current generates a debris magnetic pulse (the initial magnetic pulse), which remains attached to the expanding debris shell. Subsequently, the spatially nonmonotonically varying ambient ions velocity, characterized by an initial increase followed by a decrease, aggregates ambient ions to gradually form an ambient magnetic pulse (the second magnetic pulse). This study provides essential insights into the magnetic field evolution during the decoupling expansion and the interaction between debris and ambient plasma.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 5","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144074548","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":"Thermospheric Disturbance Observed by Triple Ionosphere PhotoMeter Onboard the Chinese Meteorological Satellite FY3E During 10–11 May 2024 Storm","authors":"Qian Song,&nbsp;Qian Ye,&nbsp;Xiaoxin Zhang,&nbsp;Tian Mao","doi":"10.1029/2024JA033386","DOIUrl":"https://doi.org/10.1029/2024JA033386","url":null,"abstract":"<p>The Triple Ionospheric PhotoMeter (TriIPM) carried on the newly launched early morning FY3E meteorological satellite measures the spectral radiances of the Earth's far ultraviolet airglow in atomic oxygen 135.6 nm (OI 135.6 nm) and N₂ Lyman-Birge-Hopfield (N₂ LBH) bands. In this paper, the TriIPM instrument data are used for the first time to record the thermospheric O/N₂ ratio variations during geomagnetic storms through the case study of the superstorm on 10–11 May 2024. The variations of the TriIPM O/N₂ ratio and the ionospheric peak density at F2 layer (NmF2) derived from the modified IRI2016 model are also compared to explore the relationship between the storm-time thermospheric and ionospheric responses. Our results show that the TriIPM O/N₂ ratio depletion extends down to the equator in the Northern Hemisphere during the main phase of the storm period. The TriIPM O/N₂ ratio depletion shows a good quantitative agreement with the NmF2 depletion within the disturbed region at a local time period between 1100 and 1900 LT. The good agreement between the TriIPM O/N₂ ratio and NmF2 indicates that the new satellite TriIPM instrument may provide a good opportunity for understanding how the thermosphere-ionosphere system responds to geomagnetic storms.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 5","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144074549","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":"Core-Halo Correlations of Solar Wind Electrons and Temperature Anisotropy Instabilities","authors":"S. M. Shaaban,&nbsp;S. Kennis,&nbsp;M. Lazar,&nbsp;V. Pierrard,&nbsp;S. Poedts","doi":"10.1029/2025JA033838","DOIUrl":"https://doi.org/10.1029/2025JA033838","url":null,"abstract":"<p>The properties of electrons in the heliospheric plasma are modulated by various factors, starting with the expansion and bimodal nature of the slow or fast solar wind, and continuing with the kinetic mechanisms of acceleration and energy exchange with small-scale plasma waves. The role of wave-particle interactions can be understood through rigorous kinetic modeling based on observational data. This paper presents a refined evaluation of the instabilities triggered by temperature anisotropy, that is, whistler and firehose instabilities, taking into account for the first time the correlations between the electron core and halo populations revealed by in situ observations. In establishing core-halo correlations, temperature anisotropies <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>(</mo>\u0000 <mi>A</mi>\u0000 <mo>)</mo>\u0000 </mrow>\u0000 <annotation> $(A)$</annotation>\u0000 </semantics></math> and plasma beta parameters <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mfenced>\u0000 <mrow>\u0000 <msub>\u0000 <mi>β</mi>\u0000 <mo>‖</mo>\u0000 </msub>\u0000 </mrow>\u0000 </mfenced>\u0000 </mrow>\u0000 <annotation> $left({beta }_{Vert }right)$</annotation>\u0000 </semantics></math> are of interest, as quantifiers of free (kinetic) energy at the origin of instabilities. These correlations incorporate the mutual effects of the electron populations and enable a realistic characterization of instabilities, in terms of either the core or the halo parameters. The instability thresholds can be significantly reduced under the mutual core-halo effects, and comparisons with observations prove the constraining role of self-generated instabilities, not only for the core but also for the halo electrons. The most relevant are the results for the slow solar wind, for which both the parameters and the core-halo correlations are less affected by the strahl component, which is otherwise more prominent in the fast wind. In high-speed winds, temperature anisotropies are more confined, most likely under a stronger effect of fluctuations generated by the electron strahl whose properties are not yet quantified to allow a similar analysis.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 5","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-05-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA033838","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143944416","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":"Ducted Propagation of Whistler Mode Waves Observed by the Arase Satellite","authors":"Y. Ampuku,&nbsp;F. Tsuchiya,&nbsp;S. Kurita,&nbsp;Y. Kasaba,&nbsp;Y. Katoh,&nbsp;M. Fukizawa,&nbsp;Y. Miyoshi,&nbsp;I. Shinohara,&nbsp;Y. Kasahara,&nbsp;S. Matsuda,&nbsp;A. Kumamoto,&nbsp;A. Matsuoka,&nbsp;M. Kitahara,&nbsp;O. Santolík","doi":"10.1029/2024JA033359","DOIUrl":"https://doi.org/10.1029/2024JA033359","url":null,"abstract":"<p>Ducted propagation of whistler-mode waves has attracted attention as a process that explains how whistler-mode waves propagate to high latitudes, resulting in the loss of relativistic electrons to the atmosphere and changes in the upper atmosphere due to electron precipitation. However, few studies have compared the observed density ducts and wave propagation characteristics to theoretical predictions in detail, particularly for low-density ducts. We present four patterns of ducting modes as electron density increases or decreases, as observed by the Arase satellite. (a) Lower-band (LB) waves propagating along a high-density duct with small wave normal angles (WNAs), (b) LB waves propagating along a low-density duct with a wide distribution of WNAs up to above the Gendrin Angle, (c) LB waves propagating along a low-density duct with WNAs around the Gendrin Angle, and (d) upper-band waves propagating along a low-density duct with small WNAs. We derived the WNAs for these cases, and their characteristics were consistent with the ducting theory. Based on this theory, we calculated the frequency range in which the waves were likely to be trapped in the ducts. We compared this frequency range with the power spectra of the recorded whistler-mode waves and found consistency between the theory and observations. Furthermore, it is suggested that the WNAs for cases (b) and (c) have azimuthal distributions based on a comparison of the WNA analysis of the simple simulated waveforms and the observed data.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 5","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-05-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JA033359","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143944417","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":"Quantifying the Impact of Whistler Waves Near the Lunar Surface Through Observational Data","authors":"Abdul Waheed,&nbsp;Zeyu An,&nbsp;Yifan Wu,&nbsp;Shangchun Teng,&nbsp;Hui Zhang,&nbsp;A. V. Artemyev,&nbsp;Xin Tao","doi":"10.1029/2024JA033628","DOIUrl":"https://doi.org/10.1029/2024JA033628","url":null,"abstract":"<p>Whistler waves are electromagnetic emissions widely observed in space plasma, and recent observational studies have confirmed their existence near the lunar surface. These waves can significantly affect the incoming plasma, causing electron heating or density depletion. However, the wave-particle interaction between the incoming solar wind and whistler waves near the lunar surface has yet to be thoroughly investigated. In this study, we employ automated methods to identify whistler wave events and investigate their statistical properties using 4 years of ARTEMIS mission data. We find that the occurrence rate and intensity of these waves are influenced by lunar magnetic field anomalies and the lunar orbital locations. To further quantify the effects of these waves, we calculate the quasi-linear diffusion coefficient based on the statistical properties of whistler mode waves near the lunar surface. Our findings indicate that these waves have intense pitch angle scattering effects on energetic electrons <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>(</mo>\u0000 <mrow>\u0000 <mn>10</mn>\u0000 <mo>−</mo>\u0000 <mn>1000</mn>\u0000 <mtext>eV</mtext>\u0000 </mrow>\u0000 <mo>)</mo>\u0000 </mrow>\u0000 <annotation> $(10-1000text{eV})$</annotation>\u0000 </semantics></math>. This study improves our understanding of the interaction between waves and particles within the plasma environment near the lunar surface.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 5","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-05-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143944500","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":"Differential Response of Nitric Oxide Radiative Cooling to Moderate and Intense Geomagnetic Storms: Insights From Superposed Epoch Analysis","authors":"Dayakrishna Nailwal,&nbsp;M. V. Sunil Krishna,&nbsp;Alok Kumar Ranjan","doi":"10.1029/2024JA033693","DOIUrl":"https://doi.org/10.1029/2024JA033693","url":null,"abstract":"<p>Geomagnetic storms have been a subject of significant interest due to their potential impact on Earth’s upper atmosphere. Nitric oxide (NO) radiative emission is a key feature that can help in understanding and assessing the storm-time response of the Earth’s upper atmosphere. This study attempts to provide a unified and comprehensive understanding of the storm-time response of NO radiative cooling to geomagnetic storms of different strengths and durations by using the superposed epoch analysis method. The satellite-based observations of NO radiative cooling at 5.3 <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>μ</mi>\u0000 </mrow>\u0000 <annotation> ${upmu }$</annotation>\u0000 </semantics></math>m during thirty geomagnetic storms have been analyzed using the superposed epoch analysis. Based on the response time of nitric oxide infrared radiative flux (NOIRF) to reach its peak value, the storms are categorized into three classes. The findings reveal that the response time of NO to a geomagnetic storm is linked to the duration of its main phase. In the case of a long-duration main-phase geomagnetic storm, the response is faster, and it is typically earlier than that during a storm with a short-duration main phase. To understand the behavior of NO during various geomagnetic storms, the temperature and compositional data from the Thermosphere Ionosphere Electrodynamic General Circulation Model (TIEGCM) simulations are used to calculate the NOIRF. The calculated NOIRF shows a good agreement with temporal variations compared to the Sounding of the Atmosphere using Broadband Emission Radiometry observations. The combined results of superposed epoch analysis and TIEGCM conclude that the duration of the main phase of a geomagnetic storm significantly affects the NO density, temperature, and response time of NOIRF.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 5","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-05-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930452","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":"Reconnection Onset in Overstretched Thin Current Sheets: PIC Simulations","authors":"M. I. Sitnov,&nbsp;H. Arnold","doi":"10.1029/2025JA033863","DOIUrl":"https://doi.org/10.1029/2025JA033863","url":null,"abstract":"<p>Onset of reconnection in the magnetotail requires its current sheet (CS) to thin down to the thermal ion gyroradius (or thinner) to demagnetize ions (or even electrons) and to provide their Landau dissipation. However, in isotropic plasma models of the tail the ion-scale CSs inflate too rapidly with the distance from Earth to remain ion-scale beyond 20 Earth's radii, where most X-lines are observed. A key to solving this problem was recently found due to the discovery of “overstretched” thin CSs (OTCSs): If an ion-scale CS is embedded into a much thicker CS with even a weak field-aligned ion anisotropy, its current density iso-contours can be stretched far beyond the magnetic field lines. Here we investigate onset of reconnection in OTCS with their scales and features closer to the observed geometry and evolution of Earth's magnetotail: extension beyond 100 ion inertial lengths, magnetic flux accumulation, dipole field effects and weak external driving. 2-D particle-in-cell (PIC) simulations with open boundaries show that OTCSs help explain the observed X-line location in the magnetotail. The reconnection electric field strongly exceeds both the external driving field and the slow convection electric field caused by the latter. The magnetic topology change (onset of reconnection proper) is preceded by divergent plasma flows suggesting that the latter are produced by the ion tearing plasma motions. OTCS are also shown to form in isotropic CS after an even shorter driving period, but their transient nature may question universality of this onset scenario.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 5","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-05-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA033863","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930230","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":"Statistical Study of Magnetic Overshoots at Collisionless Shocks","authors":"M. Lindberg,&nbsp;H. Hietala,&nbsp;K. Shirazul,&nbsp;D. Trotta,&nbsp;A. H. Sulaiman,&nbsp;B. L. Burkholder,&nbsp;A. Dimmock","doi":"10.1029/2024JA033659","DOIUrl":"https://doi.org/10.1029/2024JA033659","url":null,"abstract":"<p>We use data from the Magnetospheric Multiscale, Solar Orbiter, and Cassini spacecraft to statistically study magnetic overshoots at Earth's bow shock, interplanetary shocks, and Saturn's bow shock. The size of the magnetic overshoot exhibits a clear positive correlation with the Alfvénic Mach number and its dependence on the upstream plasma beta is investigated. We present updated empirical relationships from which the Alfvénic Mach number can be estimated using only magnetic field data via measurement of the magnetic overshoot. The magnetic overshoot and Alfvén Mach numbers are compared with a 2D hybrid simulation and previous observations at Saturn's bow shock. The comparison with Saturn displays a slight offset between the data sets. The reason for this offset is discussed and might arise from the different methods of obtaining the Mach numbers. Finally, we explore the possibility of estimating the cross-shock potential with a theoretical expression using each shock's calculated magnetic overshoot, Mach number, and plasma beta.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 5","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JA033659","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143919914","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":"Outer-Plasmasphere Plasma Hole Scenarios Promoting Hot Zone and Sub-Auroral Polarization Streams (SAPS) E Field Development","authors":"Ildiko Horvath,&nbsp;Brian C. Lovell","doi":"10.1029/2024JA033184","DOIUrl":"https://doi.org/10.1029/2024JA033184","url":null,"abstract":"<p>In this study we investigate the nightside outer-plasmasphere plasma hole developed near the magnetic equatorial plane in two different scenarios. We demonstrate the plasmasheet earthward termination with scenario-1 (on 17 and 20 February 2018) and the formation of new plasmapause by interchange motion with scenario-2 (on 22 February 2018). New findings reveal how the hot zone and the Subauroral Polarization Streams (SAPS) electric (E) field developed in the inner magnetosphere and how the underlying ionosphere became impacted in the two scenarios. In both scenarios, (a) the earthward plasma hole corresponded with the spatial extent of the hot zone where (b) plasma heating became amplified under increased ion temperature anisotropy. Fast-time SAPS E field development occurred (c) near the new plasmapause or within the plasma hole in scenario-1 and (d) across the new plasmapause in scenario-2 when SAPS E field appeared to be strongest. Via magnetosphere-ionosphere (M-I) coupling, (d) the ring-current-related ionospheric trough (RIT) and the subauroral arc developed in both scenarios. But (e) scenario-2 created more favorable conditions with the amplified downward acceleration of suprathermal electrons. From these new findings (a–e) we conclude that the inner-magnetosphere conditions, underlying the plasma hole and new plasmapause in the two scenarios investigated, were also favorable for the development of hot zone and SAPS E field and led to subauroral arc development in the coinciding SAPS channel and RIT.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 5","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2024JA033184","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143919913","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":"The Propagation and Evolution of Polar Cap Patches During Auroral Substorm Activity","authors":"Jianjun Liu,&nbsp;Yaqi Jin,&nbsp;Xiangcai Chen,&nbsp;Zhiwei Wang,&nbsp;Fang He,&nbsp;Zejun Hu,&nbsp;Akira Sessai Yukimatu,&nbsp;William Bristow,&nbsp;Hongqiao Hu,&nbsp;Beichen Zhang","doi":"10.1029/2025JA033814","DOIUrl":"https://doi.org/10.1029/2025JA033814","url":null,"abstract":"<p>Polar cap patches are islands of enhanced plasma density formed during intervals of southward interplanetary magnetic field (IMF). The present study examines the observations of polar cap patches during sequential auroral substorms that occurred on 9 September 2011. The propagation and evolution of large-scale polar cap patches were monitored by three SuperDARN radars (MCM, ZHO, and SYE) located in the Southern Hemisphere. During the substorm periods, MCM radar observed periodic blobs of anti-sunward propagating HF backscatter echoes. By examining the 2-D scan plots, there were the dawn-dusk elongated radar patches moving across the magnetic pole and eventually merging into the nightside auroral zone. Simultaneous ZHO and SYE radars recorded consecutive ionospheric plasma blobs and moderate Doppler negative velocity near the poleward boundary of the nightside auroral oval. Coordinated GPS observations in ZHO showed pulsed increases in total electron content (TEC) and scintillations. Due to the high values in the TEC data, such radar patches are suggested to result from the transportation of high-density plasma from the dayside sunlit ionosphere during sequential auroral substorms. The in situ observations by the DMSP satellite suggested re-structuring of plasma patches near the poleward boundary of the auroral oval by pulsed flow bursts.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 5","pages":""},"PeriodicalIF":2.6,"publicationDate":"2025-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA033814","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143914398","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}