Journal of Geophysical Research: Space Physics最新文献

{"title":"Effects of Strong Diffusion and Wave Ducting on Electron Losses Estimated by the Quasi-Linear Approach","authors":"Ruoxian Zhou,&nbsp;Xiao-Jia Zhang,&nbsp;Anton V. Artemyev,&nbsp;Didier Mourenas,&nbsp;Vassilis Angelopoulos","doi":"10.1029/2025JA034117","DOIUrl":"https://doi.org/10.1029/2025JA034117","url":null,"abstract":"<p>Chorus wave-driven electron precipitation into the atmosphere through pitch angle scattering plays a fundamental role in electron dynamics in the Earth's outer radiation belt. The efficiency of this precipitation is highly dependent on the wave intensity at the latitudes of resonance with electrons near the loss cone and can be directly inferred from measurements of precipitating and trapped electron fluxes measured by low-altitude satellites. In this study, we utilized statistical empirical whistler-mode chorus wave models and quasi-linear theory to simulate the precipitating electron spectrum observed by the Electron Losses and Fields INvestigation (ELFIN) CubeSats. Comparisons between simulations and observations during disturbed periods suggest the presence of a very small population of intense ducted waves, present only 5% of the time but carrying 6% (at 23-4 MLT) to 60% (at 4-12 MLT) of the total time-averaged wave power inside narrow field-aligned density ducts up to middle latitudes, and producing 20% (at 100 keV) to 60% (at 1 MeV) of the total time-integrated electron precipitation recorded by ELFIN at 23-12 MLT in 2020–2022, near or within the strong diffusion regime. Our study suggests that when modeling electron dynamics in future studies of Earth's magnetosphere or magnetosphere-ionosphere-atmosphere coupling processes, this small fraction of ducted intense chorus waves may need to be included as a separate wave population, in addition to the main wave populations typically captured in the existing empirical chorus wave models based on observations mainly performed at moderate latitudes.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272014","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":"Effective Resistivity for Magnetohydrodynamic Simulation of Collisionless Magnetic Reconnection","authors":"H. W. Zhang,&nbsp;Z. W. Ma,&nbsp;T. Chen","doi":"10.1029/2025JA034289","DOIUrl":"https://doi.org/10.1029/2025JA034289","url":null,"abstract":"<p>The electron inertia and the off-diagonal electron pressure terms are well-known for the frozen-in condition breakdown in collisionless magnetic reconnection, which are naturally kinetic and difficult to employ in magnetohydrodynamic (MHD) simulations. Considering the limitations of MHD and Hall MHD in neglecting the important electron dynamics such as the inertia and the nongyrotropic pressure, the kinetic characteristics of electrons and ions in the diffusion region are studied and an effective resistivity model involving dynamics of charged particles is proposed (Ma et al. 2018, https://doi.org/10.1038/s41598-018-28851-7 Sci. Rep. 8 10521), where the guide field is omitted to simplify the model by primarily considering the out-of-plane velocity of charged particles and the in-plane reconnecting field. The amplitude of the effective resistivity is mainly determined by electrons in most realistic situations with large ion-electron mass ratios. In this work, the effective resistivity model for collisionless magnetic reconnection is successfully applied in the 2.5D MHD and Hall MHD simulations, which remarkably improves the simulation results compared with traditional MHD models. For the MHD case, the effective resistivity significantly increases the reconnection rate to a reasonable value of <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 <mn>0.1</mn>\u0000 <msub>\u0000 <mi>B</mi>\u0000 <mn>0</mn>\u0000 </msub>\u0000 <msub>\u0000 <mi>v</mi>\u0000 <mi>A</mi>\u0000 </msub>\u0000 </mrow>\u0000 <annotation> $mathit{sim }0.1{B}_{0}{v}_{A}$</annotation>\u0000 </semantics></math>. For the Hall MHD case with effective resistivity, the peak reconnection rate is <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 <mn>0.25</mn>\u0000 <msub>\u0000 <mi>B</mi>\u0000 <mn>0</mn>\u0000 </msub>\u0000 <msub>\u0000 <mi>v</mi>\u0000 <mi>A</mi>\u0000 </msub>\u0000 </mrow>\u0000 <annotation> $mathit{sim }0.25{B}_{0}{v}_{A}$</annotation>\u0000 </semantics></math>, and the major structures of the reconnecting field and the current sheet agree well with the particle-in-cell (PIC) simulations. Meanwhile, a more general effective resistivity model incorporating guide field corrections for MHD simulations is under development.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA034289","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272015","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":"Energetic Electron Acceleration at Anti-Dipolarization Front Within the Magnetotail Reconnection Diffusion Region","authors":"Wenqing Ma,&nbsp;Zhihong Zhong,&nbsp;Hui Zhu,&nbsp;Meng Zhou,&nbsp;Ye Pang","doi":"10.1029/2025JA034376","DOIUrl":"https://doi.org/10.1029/2025JA034376","url":null,"abstract":"<p>Anti-dipolarization front (ADF), characterized by the sharp increase of the southward magnetic field (<i>B</i>_<i>Z</i>,GSM &lt; 0), is a magnetic structure with reconnected magnetic field enhancement in the magnetotail reconnection. It is considered to be an important region for energy conversion in the tailward reconnection jet. In this paper, we report an ADF event within the magnetotail reconnection diffusion region, which may comprise two ADFs and exhibit a significant enhancement of energetic electron flux. We analyze the corresponding electron acceleration mechanisms and find that the Fermi acceleration dominates the local electron energy gain, contributing to the production of energetic electrons. The magnetic mirror effect and large-scale parallel electric potential may effectively trap the energetic electrons and facilitate Fermi acceleration. Our study provides important information for further understanding the mechanisms of energetic electron generation in space plasma.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145272062","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":"Parametric Dependence of Linear and Nonlinear Growth of Whistler-Mode Chorus Waves","authors":"Tian Zhang,&nbsp;Yusuke Ebihara,&nbsp;Yoshiharu Omura","doi":"10.1029/2025JA034244","DOIUrl":"https://doi.org/10.1029/2025JA034244","url":null,"abstract":"<p>We calculated the linear and nonlinear growth rates of whistler-mode chorus waves with relativistic treatment across different wave frequencies and investigated their dependence on the associated parameters, including background magnetic field strength, cold electron density, and energetic electron temperature. The linear and nonlinear growth rates, with respect to any of the three parameters in the range investigated, are confirmed to often exhibit a peak, at least, in the lower band (i.e., &lt;0.5 <i>f</i>_ce, electron cyclotron frequency). For a given energetic electron temperature between 0.5 and 500 keV, both linear and nonlinear growth rates at low frequencies can be positive in a specific range of background magnetic field strength and cold electron density, with an optimum growth rate occurring when either parameter is fixed. However, as the electron temperature increases within this range, linear damping becomes more pronounced, resulting in a suppression of linear growth at high frequencies. On the other hand, as the strength of the magnetic field increases, a higher energetic electron temperature is required to sustain wave growth. Notably, nonlinear growth can still occur even when the linear growth rate is negative as previous studies have demonstrated. Parameters leading to such conditions are also demonstrated. Comparisons with previous chorus wave observations confirm the dependence on the parameters and explain the existence of an optimum wave growth condition and overlapping parameter ranges for both linear and nonlinear wave growth.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA034244","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145271672","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":"Enhanced Radiation at Aviation Altitudes and Plasmaspheric Hiss Waves—A Time Shift Analysis","authors":"Homayon Aryan,&nbsp;Jacob Bortnik,&nbsp;W. Kent Tobiska,&nbsp;Piyush Mehta,&nbsp;Benjamin Hogan,&nbsp;Harshitha Challa","doi":"10.1029/2025JA033959","DOIUrl":"https://doi.org/10.1029/2025JA033959","url":null,"abstract":"<p>Increased radiation levels in Earth's atmosphere can present significant risks to airline pilots, passengers, and commercial space travelers. Recent findings have revealed a strong statistical link between radiation dose rates detected at aviation altitudes (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>&gt;</mo>\u0000 <mn>9</mn>\u0000 </mrow>\u0000 <annotation> ${ &gt;} 9$</annotation>\u0000 </semantics></math>km) and plasmaspheric hiss wave power observed along the same magnetic field lines within the inner magnetosphere. Plasmaspheric hiss waves are crucial in depleting energetic electrons from Earth's radiation belts by causing them to precipitate into the upper atmosphere. In this study, we examine magnetic conjunction events between the Automated Radiation Measurements for Aerospace Safety (ARMAS) instruments and the Van Allen Probes to explore the relationship between plasmaspheric hiss waves and enhanced radiation at aviation altitudes. Specifically, we focus on how variations in conjunction timing, together with shifts in L-shell, and Magnetic Local Time influence the correlation between radiation dose rates and plasmaspheric hiss wave power. This investigation aims to determine whether the observed increase in radiation at aviation altitudes is directly linked to plasmaspheric hiss waves within the inner magnetosphere and to explore the extent to which enhanced radiation due to plasmaspheric hiss waves is localized in space and time. Results show that the strongest cross-correlation is only observed when plasmaspheric hiss waves and radiation doses occur nearly simultaneously and with close proximity. Spatiotemporal variations result in a degradation of the observed correlation.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA033959","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145271708","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":"Occurrence Rates and Variability of Whistler-Mode Waves in the Plasma Trough","authors":"C. E. J. Watt,&nbsp;N. P. Meredith,&nbsp;J. Wong,&nbsp;K. R. Murphy,&nbsp;I. J. Rae,&nbsp;S. Chakraborty,&nbsp;S. N. Bentley,&nbsp;O. Allanson,&nbsp;C. J. Rodger","doi":"10.1029/2025JA034061","DOIUrl":"https://doi.org/10.1029/2025JA034061","url":null,"abstract":"<p>Numerical models of energetic electron behavior in the outer radiation belt require descriptions of the wave-particle interactions across the inner magnetosphere. Quasilinear diffusion coefficients describe gyro-resonant wave-particle interactions over large time- and length-scales but these must be constrained by observations to construct realistic radiation belt models. Recent work indicates the importance of identifying and including realistic spatiotemporal variation of diffusion coefficients. In this paper, we study the spatiotemporal variability of whistler-mode waves outside the plasmasphere, typically referred to as whistler-mode chorus. We separately consider the probability of (a) parts of the model domain being outside the plasmasphere, and (b) the probability of detecting wave activity should that part of the model domain be outside the plasmasphere. We discover that the spatiotemporal variability of whistler-mode waves significantly differs across the model domain; we propose that wave power variability in short wave intervals (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 <mn>5</mn>\u0000 </mrow>\u0000 <annotation> ${sim} 5$</annotation>\u0000 </semantics></math> min) is a useful characteristic to distinguish between two types of whistler-mode waves, especially where their frequency ranges overlap. Our novel spatiotemporal variability analysis indicates that low variability waves are dayside exohiss whose typically high occurrence rate (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mo>∼</mo>\u0000 <mn>0.8</mn>\u0000 </mrow>\u0000 <annotation> ${sim} 0.8$</annotation>\u0000 </semantics></math>) decreases with substorm activity, and high variability waves are sporadic post-midnight/dawn sector substorm-driven chorus with a typical occurrence rate of 0.2. Further, although previous studies often combine the occurrence rates and wave characteristics into climatological averages of chorus wave power, this study highlights the importance of separating the study of occurrence rates and power of the waves, since each can have a different relationship with driving factors.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA034061","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145224324","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":"A Specification Model of Saturn's Plasma Environment","authors":"A. Kamran,&nbsp;Q. Nénon,&nbsp;F. L. Johansson,&nbsp;Y. Hao,&nbsp;A. Sicard,&nbsp;E. Roussos,&nbsp;K. Dialynas,&nbsp;P. Jiggens,&nbsp;F. Cipriani","doi":"10.1029/2025JA034005","DOIUrl":"https://doi.org/10.1029/2025JA034005","url":null,"abstract":"<p>We present the first empirical-based specification model of Saturn's plasma environment based on the analysis of all publicly available plasma moment data sets derived using multiple techniques from Cassini observations made by the Cassini Plasma Spectrometer and the Radio and Plasma Wave Science instrument. We investigate the variability of the plasma moments with respect to minimum normal distance to the current sheet, L-shell, magnetic latitude, and magnetic local time, and find the latter three parameters to be the most useful to construct the long-term average configuration of plasma moments in Saturn's magnetosphere. The model moments generated by the model include electron and ion densities, temperatures and ion velocities. Given that the majority of the analyzed plasma data are constrained to the equatorial region of Saturn's magnetosphere, we also present an example of extending the plasma model to larger latitudinal ranges with a physics-based extrapolation related to plasma equilibrium. This model will be used to support future space mission planning and development for the Saturnian system, as the moon Enceladus, a planetary body that meets the major criteria for habitability, has been highlighted as a top target for large-scale space missions by various space agencies.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA034005","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145224056","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":"Emission of Energetic Neutral Atoms From Ganymede's Magnetosphere-Atmosphere Interaction","authors":"C. Michael Haynes,&nbsp;Sven Simon,&nbsp;Lucas Liuzzo","doi":"10.1029/2025JA034469","DOIUrl":"https://doi.org/10.1029/2025JA034469","url":null,"abstract":"<p>This study analyzes the emission of energetic neutral atoms (ENAs), generated by charge exchange between energetic protons and Ganymede's atmosphere. We also constrain the observability of such ENAs by an imaging instrument aboard a spacecraft. Our approach employs tracing tools that calculate the trajectories of magnetospheric parent protons near Ganymede. We determine the ENA flux through a hypothetical spherical detector encompassing the moon's atmosphere. We additionally generate synthetic ENA images, as seen by a point-like detector with a finite field of view. The complexity of Ganymede's electromagnetic environment is successively increased; we consider (i) uniform Jovian fields, (ii) the superposition of the moon's internal dipole with Jupiter's field, and (iii) draped fields from a hybrid model of Ganymede's plasma interaction. Our major results are: (a) In uniform fields, the ENA flux is elevated within a circular band on the detector sphere. Synthetic ENA images record a cluster of high flux near the moon's limb, with the position of this enhancement determined by the viewing geometry. (b) When including Ganymede's internal dipole, the flux through the sphere displays a localized increase above the ramside apex, mainly generated by protons on open field lines at mid-latitudes. In the synthetic images, the reduced ENA emissions from the closed field line region produce local flux depletions along the equator. (c) Pile-up of Jupiter's field significantly reduces the ENA flux from Ganymede's ramside atmosphere. (d) At energies above several keV, the emissions from Ganymede's atmosphere clearly exceed the ENA flux released from the moon's surface.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2025JA034469","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145224067","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":"Latitudinal Profiles of Nightside Isotropy Boundaries: Comparison of Observations and Predictions of Adaptive Magnetospheric Model","authors":"V. A. Sergeev,&nbsp;M. V. Kubyshkina,&nbsp;I. V. Kubyshkin,&nbsp;A. Artemyev,&nbsp;V. Angelopoulos","doi":"10.1029/2025JA034428","DOIUrl":"https://doi.org/10.1029/2025JA034428","url":null,"abstract":"<p>There is significant interest in monitoring the instantaneous magnetic configurations and dynamic states of the magnetotail and understanding what controls them. A unique and attractive opportunity is provided by remote sensing of the radial profile of the equatorial magnetic field curvature based on low-latitude energetic particle measurements of isotropy boundaries (IBs), providing that you can determine the origin of isotropic precipitation. To validate the magnetic field line curvature scattering (FLCS) as the main mechanism of the isotropy boundary formation, we compare coarse energy versus latitude IB profiles (in 3 + 3 energy channels) measured during a few dozen passes of POES and ELFIN spacecraft with the theoretical predictions of the adapted (AM03) magnetospheric model. Two studied intervals in August 2022 include substorm events of various intensities for which good spacecraft coverage in the near magnetotail helps reconstruct the adaptive model in the areas where the IBs are formed. We find a general agreement between the predicted and observed <i>coarse</i> IB profiles' shape and latitude, validating the FLCS hypothesis. Deviations are also observed, and we discuss the factors that can influence identification of the true FLCS profiles in observations and predictions, including limitations of adaptive modeling, non-monotonic radial structure of the tail magnetic field, and interference of FLCS with other precipitation mechanisms related to wave-particle interactions. Most can be avoided by improving the sensitivity, energy coverage, and resolution in future instruments.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145224065","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":"Wisp-Like Energy Spectrum of Precipitating Electrons Observed by DEMETER Satellite","authors":"Jingle Hu,&nbsp;Binbin Ni,&nbsp;Yangxizi Liu,&nbsp;Junhu Dong,&nbsp;Jianhang Wang,&nbsp;Haozhi Guo,&nbsp;Jiakun Dai,&nbsp;Zheng Xiang","doi":"10.1029/2025JA034457","DOIUrl":"https://doi.org/10.1029/2025JA034457","url":null,"abstract":"<p>Very-low-frequency (VLF) signals used for submarine communication can penetrate the ionosphere and leak into the magnetosphere. These signals interact with hundreds of keV electrons in the inner magnetosphere through cyclotron resonance, resulting in pitch angle diffusion of trapped electrons. The energy-<i>L</i> spectrum of quasi-trapped electrons (in the drift loss cone scattered by North West Cape (NWC) transmitted signals in the inner radiation belt is called “wisp,” characterized by narrow spectral peaks of enhanced fluxes. These quasi-trapped electrons drift eastward and can be clearly observed by Low-Earth-Orbit satellites until they precipitate into the South Atlantic Anomaly (SAA) region, where they drift into the bounce loss cone (BLC). The transmitter-induced BLC precipitation with a wisp structure has been considered uncommon. In this study, we report the direct and clear observational evidence of transmitter-induced precipitating wisps which are commonly observed at the edge of the northern hemisphere precipitation regions (the regions conjugated to the SAA). Moreover, we systematically analyze the dependence of these electron fluxes on <i>L</i>-shell, electron energies and geomagnetic activities, using long-term measurements from the DEMETER satellite. The intensities and positions of the precipitating wisps in the energy-<i>L</i> spectrum are highly correlated with the quasi-trapped wisps. The visible wisp structure in the precipitating electrons can only be detected when the quasi-trapped electron fluxes exceed a certain threshold ∼10³ cm⁻²ster⁻¹s⁻¹ MeV⁻¹. The overall variation in precipitating electron fluxes follows the trend observed in trapped electron fluxes. These results provide new insights into the quantitative scattering effects of NWC transmitter signals on energetic electrons.</p>","PeriodicalId":15894,"journal":{"name":"Journal of Geophysical Research: Space Physics","volume":"130 10","pages":""},"PeriodicalIF":2.9,"publicationDate":"2025-10-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145223783","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}