Energetic Electron Dynamics are ones of the most dynamic processes in Earth's magnetosphere and have global consequences and broad implications for space weather. They can be monitored using energetic electron detectors on both Macao Science Satellites (MSS-1A/B) and sunsynchronous satellites (Fengyun 3E). There are triple Imaging Electron Spectrometer (IES)  instruments to be installed in the Macao Science Satellites and Chinese Sun-synchronous (FY3E) satellites, respectively. The IES instrument on board  both Macao Science Satellites and Chinese Meteorology FY-3 (sunsynchronous) satellite, launched on May, 2023, and 4 July, 2021 (FY-3)  into a sunsynchronous satellite orbit (LEO), provides the first  constellation eneregetic electron measurements in the inner Radiation Belt and SAA region. The Macau Scientific Satellite - 1 (MSS) comprises two satellites orbiting the Earth at an inclination of 41. MSS1-A follows a circular orbit at an altitude of 450 km, while MSS1-B's orbit is elliptical, ranging between 450 and 500 km in altitude, with its apogee positioned near the South Atlantic Anomaly (SAA). These two satellites share a similar orbit, maintaining a separation of approximately 5-10s minutes, which has varied since their launch. The orbital period for both satellites is approximately 94 minutes.  The innermost and outermost signatures of substorm injection have been observed by the IES instruments with a wide L shell spatial coverage, from L=1 ~ 6.  Such a configuration will provide a unique opportunity to investigate Energetic Electron Dynamics simultaneously at low and high  L shells. It will further elucidate potential mechanisms for the particle energization and transport, two of the most important topics in inner radiation belt dynamics.  

How to cite: Zong, Q.: Energetic Electron Dynamic in the Inner Radiation Belt and SAA Region, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-18185, https://doi.org/10.5194/egusphere-egu24-18185, 2024.

The Relativistic Electron-Proton Telescope (REPT) Pulse Height Analysis (PHA) data captures individual particle event for each of REPT’s nine silicon detectors onboard the Van Allen Probes. The PHA data set was taken every 12 milliseconds (ms), including the pulse height that is proportional to the energy deposit of each individual particle from all nine detectors. Geant4 simulations are used to extend and improve the electron detecting capabilities of REPT (beyond its nominal data) using the PHA data. After replicating the nominal characteristics of REPT in the Geant4 toolbox, new channels for REPT, going from 12 nominal electron channels to 47 and lowering the minimum energy to ~1 MeV, have been formulated. By applying these newly simulated electron channels to PHA data and combining with the detector singles rates, an estimated count rate data product for finer-resolution, lower-energy channels is created. This method enables higher resolution observations of electrons of 1.1 – 12 MeV, revealing more detailed characteristics of these high energy electrons in the magnetosphere, especially in the inner edge of the outer belt, slot region, and inner belt. Similarly, Relativistic Electron and Proton Telescope integrated little experiment -2 (REPTile-2) onboard Colorado Inner Radiation Belt Experiment (CIRBE), launched on 15 April 2023 into a low Earth orbit (LEO), has implemented PHA processing onboard, measuring 0.25 – 6 MeV electrons in 60 channels and protons in 60 channels and revealing detailed structures of the energetic electrons and protons, especially in the inner belt.

How to cite: Li, X., O'Brien, D., Mei, Y., Xiang, Z., and Baker, D.: Observations and Analysis of MeV Electrons from REPT PHA Data and REPTile-2 data , EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-2493, https://doi.org/10.5194/egusphere-egu24-2493, 2024.

The Arase satellite observes the dynamics of the Earth’s radiation belts, including the electron fluxes over a wide energy range from a few electronvolts to several MeV. This work focuses on the measurements of the Arase high-energy electron experiment (HEP), specifically its instrument HEP-L that observes electrons from 60 keV to 1.5 MeV. It is a state-of-the-art instrument capable of distinguishing the incoming direction of electrons by position sensitive detectors, thus accurately determining the pitch angle. HEP-L has been previously calibrated based on the modeled response functions of the instrument’s energy channels using Geant4 simulation. The current work utilizes the same simulation, but now considering the calibration in terms of the azimuthal channels, i.e., the direction of measured counts. As shown by the simulation, the distribution of counts in each azimuthal channel is broader than the nominal range in the initial direction angle, causing cross-channel contamination. We propose a new method to calibrate HEP-L data to diminish this contamination, and applying the correction method lowers the electron fluxes especially at field-aligned pitch angles, where uncorrected HEP-L data were overestimated, as seen in comparison with other instruments on board Arase and the Van Allen Probes. Pitch angle distributions (PADs) from Arase and Van Allen Probes were compared during close conjunctions of the spacecraft. Previous comparisons have only considered the omnidirectional fluxes which offer a limited view of the radiation belt dynamics. PADs provide a more detailed comparison and shed light on, e.g., wave-particle interactions. Here we derived PADs from HEP-L and extremely high-energy experiment (XEP) on Arase, and the Magnetic Electron Ion Spectrometer (MagEIS) and the Relativistic Electron-Proton Telescope (REPT) instruments on Van Allen Probes to cover a large energy range. There is a remarkable agreement within a factor of 2 for all energies, for all pitch angles for XEP data and for most pitch angles (20 to 160 degrees) for uncorrected HEP-L data. By applying the new correction, the discrepancy at the field-aligned pitch angles is reduced.

How to cite: Kalliokoski, M., Asamura, K., Shinohara, I., Mitani, T., Hori, T., Miyoshi, Y., Higashio, N., and Takashima, T.: Arase HEP-L electron measurement calibration and comparisons of pitch angle distributions with Van Allen Probes, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-5770, https://doi.org/10.5194/egusphere-egu24-5770, 2024.

Substorms and strong convection events occurring during high-intensity long-duration continuous auroral electrojet (AE) activity (HILDCAA) events are associated with acceleration of magnetospheric relativistic electrons. From an analysis of Van Allen Probe satellite measurements, it is shown that ~7 MeV electrons are accelerated during ~3.4–4.1 days-long HILDCAA events. The dominant acceleration process is due to wave-particle interactions between magnetospheric electromagnetic chorus waves and substorm injected ~100 keV electrons. The longer the HILDCAA and chorus last, the higher the maximum energy of the accelerated relativistic electrons. The acceleration to higher and higher energies is by a bootstrap mechanism. Due to the unusually long process associated with the electron acceleration to ~7 MeV, spacecraft controllers can be given proper advance warning to shift to other modes of operation for the protection of spacecraft electronics.

How to cite: Hajra, R., Tsurutani, B., Lu, Q., Lakhina, G., and Du, A.: Ultra-relativistic 7 MeV electron acceleration during intense and long-duration substorm activity, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-1352, https://doi.org/10.5194/egusphere-egu24-1352, 2024.

Electron radiation belt enhancement events are a key phenomena of the Earth geomagnetic activity and have been thoroughly studied in the literature.

Establishing extensive catalogs of these events automatically is a key asset to both the global statistical study of the electron radiation belt enhancement and, from an operational perspective, to provide actionable scenario-based forecasts. The latter being the objective of the EU Horizon Europe FARBES (Forecast of Actionable Radiation Belts Scenarios) under which this work is funded.

Nowadays, the existing attempts of establishments of such catalogs are scarce and often based on the exceedance of certain thresholds of ground-based measurements (Bernoux and Maget, 2020) or onboard electron fluxes (Reeves et al. 2020). Which often leads to missed events, non-events or events with unrealistic boundaries.

In this work, we introduce a novel automatic detection method of radiation belt enhancement events based on the Ca index (Rochel et al. 2016), a simple 1D-proxy representative of the state of the electron radiation belts for average energies (up to  MeV). This method is then used to produce an extensive catalog of events between 1870 and 2023 with more realistic boundaries. The most recent events of this catalog (detected after 1995) are then associated with their possible physical cause, whether it be Interplanetary Coronal Mass Ejections (ICMEs) or Streaming-Interaction regions (SIRs).

How to cite: Nguyen, G., Bernoux, G., and Maget, V.: Introducing a new ground-based Radiation belt electron enhancement events catalog, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-7584, https://doi.org/10.5194/egusphere-egu24-7584, 2024.

Radial diffusion, driven by Ultra-Low Frequency (ULF) waves in the Pc4–5 band (2–25 mHz), has been established as one of the most important mechanisms that influences the dynamics of electrons in a quite broad energy range, as it can lead to both energization and loss of relativistic electrons in the outer Van Allen radiation belt. The same has been observed in other planetary magnetospheres. The dependence of ULF wave power spectral density and radial diffusion coefficients (D_LL) on solar wind parameters has been investigated by some studies, but their relationship on the various solar and interplanetary drivers is far from well-studied and understood. In this study, we use the “SafeSpace” database (https://synergasia.uoa.gr/modules/document/?course=PHYS120), which contains radial diffusion coefficients and ULF wave power spectral density, and was created using magnetic and electric field measurements from the THEMIS satellites in the 2011–2019 time-period. We conduct an extensive statistical analysis of D_LL in order to investigate the relationships between the magnetic and electric components as well as their dependence on interplanetary drivers (i.e. High Speed Streams and Interplanetary Coronal Mass Ejections). Our results reveal an energy dependence of the radial diffusion coefficients as well as significant variations of the D_LL spectral profiles as a function of Roederer’s L*. Our findings highlight statistical, as well as physical, characteristics and aspects of D_LL which are not included in most semi-empirical models typically used in radiation belt simulations, thus potentially introducing significant biases in the estimation of the outer belt relativistic electron environment. Further discussion will be devoted to the uncertainties of such efforts as well as the possible contribution of magnetosheath processes (e.g., jets and electron injections from the foreshock) and solar wind mechanisms (periodic density structures).

The work leading to this paper has received funding from the European Union’s Horizon Europe research and innovation programme under grant agreement No 101081772 for the FARBES (Forecast of Actionable Radiation Belt Scenarios) project.

How to cite: Katsavrias, C., Aminalragia-Giamini, S., Thanasoula, K., Nasi, A., Papadimitriou, C., Georgiou, M., Balasis, G., and Daglis, I. A.: ULF waves in geospace and the challenge of estimating radial diffusion coefficients from in situ data., EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-14967, https://doi.org/10.5194/egusphere-egu24-14967, 2024.

How to cite: Yan, L., Liu, W., Zhang, D., Sarris, T. E., Li, X., Tong, X., and Cao, J.: Cluster Observation on the Latitudinal Distribution of Magnetic Pc5 Pulsations in the Inner Magnetosphere, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-5101, https://doi.org/10.5194/egusphere-egu24-5101, 2024.

Electron resonant interaction with ultra-low-frequency (ULF) waves is the one of the main drivers of the electron radial transport in the Earth's inner magnetosphere. Recent spacecraft observations reported a possibility for electrons to resonate nonlinearly with intense coherent ULF waves, way beyond traditional approach of a slow diffusive scattering of electrons by a broad-band ULF spectrum. In this study we propose a theoretical model describing key elements of such nonlinear resonant interactions. We adapted the Hamiltonian approach to describe equatorial electron motion in the dipole magnetic field and electric ULF wave field. We demonstrated the presence of two main regimes for ULF-electron interaction: the phase bunching and phase trapping. We discuss possible applications of the proposed theoretical approach and the importance of ULF-electron nonlinear resonance. 

How to cite: Vainchtein, D., Artemyev, A., and An, X.: Hamiltonian approach to the electron resonant interaction with coherent ULF waves, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-6588, https://doi.org/10.5194/egusphere-egu24-6588, 2024.

By using the magnetic field data from Van Allen Probes, we analyzed the distribution characteristics of the electromagnetic environment in the inner magnetosphere on different Dst* index and magnetic local time. Our results show that for the response of different current systems, the dawn-dusk and noon-midnight asymmetry distribution of the residual magnetic field δB increases with Dst* index. When Dst* < −60 nT, a “banana”-shaped geomagnetic field negative disturbance peak region appears in the sector from midnight to dusk. Then, we obtained the azimuthal current density and found the asymmetric internal eastward and external westward ring current. Through the vector analysis of three-dimensional current density, the current density vector distribution in the magnetic equatorial plane is completely displayed for the first time, which directly proves the existence of banana current near r = 3.0–4.0 R_E during strong geomagnetic storms.

How to cite: Zhang, X.-X., Wang, T., He, F., Lv, J., Zong, Q., and Fu, H.: Banana Current in the Inner Magnetosphere Observed by Van Allen Probes, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-2562, https://doi.org/10.5194/egusphere-egu24-2562, 2024.

The Earth's magnetosphere is a dynamic system subject to various disturbances, among which substorms play a significant role in influencing its impact on the surrounding plasma environment. Close to the substorm onset satellites flying in the night side often observe reconfiguration of magnetic field lines from tail like to quasi-dipole like. This phenomenon is called magnetic field dipolarization. Studying the particle and wave dynamics during this phenomenon is crucial to understand as it accelerates the ion population and alters the generation condition of waves associated with it. Using the Electric and Magnetic Field Instrument Suite (EMFISIS) onboard the Van Allen Probes spacecraft, the present study investigates the magnetic field fluctuations corresponding to substorm onset. We examine thirteen substorm occurrences with L < 6.6 and within wide a range of MLT (18:00 to 06:00). Our investigation reveals significant magnetic field fluctuations exhibiting power from gyrofrequency of O⁺ extending up to gyrofrequency of H⁺. We additionally calculate the plasma and magnetic pressures, providing insight into the mechanism triggering ion injection during these occurrences. The role of heavy ions (He⁺ and O⁺) in the disappearance of stop bands and the corresponding mechanisms involved in this phenomenon it will we presented.

How to cite: Shah, T., Bhaskara, V., Omura, Y., Ojha, B., Singh, S., and Ebihara, Y.: Plasma wave occurrences during substorm events , EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-17365, https://doi.org/10.5194/egusphere-egu24-17365, 2024.

The geospace plume, referring to the combined processes of the plasmaspheric and the ionospheric storm-enhanced density (SED)/total electron content (TEC) plumes, is one of the unique features of geomagnetic storms. The apparent spatial overlap and joint temporal evolution between the plasmaspheric plume and the equatorial mapping of the SED/TEC plume indicate strong magnetospheric-ionospheric coupling. However, a systematic modeling study of the factors contributing to geospace plume development has not yet been performed due to the lack of a sufficiently comprehensive model including all the relevant physical processes. In this paper, we present a numerical simulation of the geospace plume in the March 31, 2001 storm using the Multiscale Atmosphere Geospace Environment model. The simulation reproduces the observed linkage of the two plumes, which, we interpret as a result of both being driven by the electric field that maps between the magnetosphere and the ionosphere. The model predicts two velocity channels of sunward plasma drift at different latitudes in the dusk sector during the storm main phase, which are identified as the sub-auroral polarization streams (SAPS) and the convection return flow, respectively. The SAPS is responsible for the erosion of the plasmasphere plume and contributes to the ionospheric TEC depletion in the midlatitude trough region. We further find the spatial distributions of the magnetospheric ring current ions and electrons, determined by a delicate balance of the energy-dependent gradient/curvature drifts and the E´B drifts, are crucial to sustain the SAPS electric field that shapes the geospace plume throughout the storm main phase.

How to cite: Bao, S., Wang, W., Sorathia, K., Merkin, V., Toffoletto, F., Lin, D., Pham, K., Garretson, J., Wiltberger, M., Lyon, J., and Michael, A.: Understanding the inner magnetospheric drivers of the geospace plume evolution through magnetosphere-ionosphere coupling, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-2660, https://doi.org/10.5194/egusphere-egu24-2660, 2024.

A long-standing question in studying the plasma dynamics in the magnetosphere pertains to the mass coupling between the ionosphere and the global magnetosphere. This presentation explores the connection between different plasma populations lying within and outside the magnetosphere, and employs an integrated computational approach to model the geospace environment, enabling a comprehensive analysis of the evolution of all significant heavy ion species. 

In this presentation, we explore the circulation patterns, transport, and energization of heavy ions as they are transported from the high-latitude ionosphere across the expansive magnetosphere, examining their influence on the dynamics of the inner magnetospheric plasma. Moreover, we present compelling evidence indicating that the presence of energetic heavy ions in the inner magnetosphere significantly contributes to the initial stages of plasmasphere refilling. This contribution stems from the composition of heavy ions within the plasma sheet, which primarily dictates the formation of cold protons through charge exchange with the geocorona, with the neutral density exerting a comparatively minor role. 

How to cite: Ilie, R. and Liu, J.: How the ionosphere is shaping the dynamics of the near-Earth plasma: Insights into mass coupling across the magnetosphere, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-20829, https://doi.org/10.5194/egusphere-egu24-20829, 2024.

The drift-bounce resonance between ultralow-frequency (ULF) wave and charged particles is an efficient way to transfer energy. In this study, we report the excitation of ULF waves through drift-bounce resonance with protons in the magnetic dip for the first time. On 4 September 2015, Van Allen probe B observed ULF signals with a frequency of ~10 mHz inside the magnetic dip during substorms at the dusk side. The ULF waves are further diagnosed as second harmonic poloidal waves. The 54-67 keV protons in the magnetic dip exhibit oscillations with the same period as ULF waves, providing evidence for drift-bounce resonance. Through finite Larmor radius effects combined with simulations, we determined the ULF waves propagate eastward with an azimuthal wave number of ∼240. The sign of df/dW reveals that the ULF waves are excited and related to the outward radial gradient of proton phase space density. 

How to cite: Zhuang, Y., Yue, C., Li, L., Zhou, X.-Z., Zong, Q.-G., Li, X.-Y., Yin, Z.-F., Liu, Y., Fu, H., Liu, Z.-Y., and Wang, Y.-F.: The Excitation of Eastward Second Harmonic Poloidal Waves Through Drift-Bounce Resonance with Protons in the Magnetic Dip, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-9438, https://doi.org/10.5194/egusphere-egu24-9438, 2024.

The present study uncovers the fine structures of magnetosonic waves by investigating the EFW waveforms measured by Van Allen Probes. We show that each harmonic of the magnetosonic wave may consist of a series of elementary rising-tone emissions, implying a nonlinear mechanism for the wave generation. By investigating an elementary rising-tone magnetosonic wave that spans a wide frequency range, we show that the frequency sweep rate is likely proportional to the wave frequency. Furthermore, we reveal that each elementary rising-tone magnetosonic waves consist of multiple mini-harmonics spaced at O+ gyrofrequency. We reveal that O+ ions can suppress the generation of magnetosonic waves at multiples of O+ gyrofrequency, resulting in the mini-harmonic structure. The commonly observed mini-harmonics indicate an energy transfer between different ion species.

How to cite: Li, J., Bortnik, J., Tian, S., and Ma, Q.: Fine structures of magnetospheric magnetosonic waves: elementary rising-tone emissions and mini harmonics, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-4923, https://doi.org/10.5194/egusphere-egu24-4923, 2024.

The intensity of magnetospheric whistler-mode waves at frequencies of a few kilohertz sometimes exhibits nearly periodic temporal or frequency modulation. Events exhibiting temporal modulation are typically referred to as quasiperiodic (QP) emissions, while those with frequency modulation are commonly known as magnetospheric line radiation (MLR). Although these events are rather routinely observed both by spacecraft and ground-based instruments, their exact formation mechanism is still not fully understood.

We use high-resolution burst mode data, measured by the Van Allen Probes spacecraft in the equatorial region at larger radial distances, by the low-altitude DEMETER spacecraft, and by the Kannuslehto and PWING ground-based instruments, to demonstrate and investigate the fine inner structure of these events. We show that such a fine inner structure is often present for both QP and MLR events. Detailed wave propagation and timing analysis reveals that it corresponds to the wave bouncing between the hemispheres. We discuss the possible implications of these observations for understanding the event formation mechanisms.

How to cite: Němec, F., Santolík, O., Manninen, J., Martinez-Calderon, C., Shiokawa, K., Hospodarsky, G. B., and Kurth, W. S.: Whistler-mode quasiperiodic emissions and magnetospheric line radiation: Fine inner structure, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-8984, https://doi.org/10.5194/egusphere-egu24-8984, 2024.

Whistler-mode chorus waves play an important role to control electron dynamics in the Earth’s radiation belt. Most of the existing theoretical and simulation studies on the chorus waves assume a one-dimensional field-aligned wave propagation. Physics of the chorus wave excitation and evolution in the multi-dimensional dipole field geometry still remains a challenge. The oblique propagation will be subject to wave attenuation at higher latitudes and introduce additional harmonic resonances. We have conducted simulations of two-dimensional chorus waves excited by hot anisotropic electrons interacting with cold dense plasma in a dipole magnetic field. It is found that the rising tone element of chorus waves with frequency chirping from low frequency to up to higher than the half electron gyro-frequency is generated at low latitudes. As the chorus wave propagates toward high latitudes, the wave becomes oblique and both the Landau and cyclotron resonance become significant. Two bands chorus waves are thus formed. In addition, we have found that a strong wave-particle interaction process presents in multi-dimensional electron distribution during the formation of chorus wave subpackets. The nonlinear physics associated with the wave growth and wave frequency chirping has been quantitatively evaluated in the process of chorus wave development.

How to cite: Wang, X., Omura, Y., Chen, H., Hsieh, Y., Lin, Y., and Chen, L.: Simulation Study of Whistler-Mode Chorus Wave Generation in the Earth's Inner Magnetosphere, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-1264, https://doi.org/10.5194/egusphere-egu24-1264, 2024.

In this study, we investigate Poynting fluxes of plasmaspheric hiss waves using the Van Allen Probes wave observation. The hiss waves are identified based on the number density of cold plasma, wave frequency, ellipticity, wave normal angle, and planarity. The statistical results show that on the dayside the Poynting flux magnitudes of the hiss waves are stronger than those on the nightside and their field-aligned components are much larger than the perpendicular components. We calculate the net Poynting flux direction R_s of hiss waves along field-aligned direction for different frequency ranges, under different geomagnetic activities, and in different MLT sectors, whose sign can indicate the balance between the growth and damping processes. We find that in the inner plasmasphere R_s is negative while in the outer plasmasphere R_s is positive and their transition locations significantly depend on wave frequency and geomagnetic activity. The results suggest that the local generation of hiss waves may be important in the outer plasmasphere. 

How to cite: Zhu, H., Chen, H., and Lu, M.: On the field-aligned Poynting fluxes of plasmaspheric hiss, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-6644, https://doi.org/10.5194/egusphere-egu24-6644, 2024.

How to cite: Ma, L., Yu, Y., Tong, X., Tang, L., Liu, W., Cao, J., Wu, J., and Wu, J.: Ionospheric responses modulated by quasi-periodic EMIC waves associated with ULF waves, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-4512, https://doi.org/10.5194/egusphere-egu24-4512, 2024.

Recent work revealed the existence of plasmapause surface waves (PSWs) with Van Allen Probes observations, which are characterized by the periodic modulations of both magnetic/electric fields and plasma densities, and suggested to be the driver of giant undulations (GUs). In this study, six years data from Van Allen Probes were used to investigate the spatial distributions and occurrence conditions of PSWs in the period of 5–30 min. PSWs are found to be mainly distributed at L = 3.5–7 and their occurrence rate is increasing with larger L shells. In the azimuth direction, the spatial distribution of PSWs exhibits an obvious dawn-dusk asymmetry with highest occurrence rates at MLT = 15–21, which is consistent with the spatial distribution of GUs revealed in the previous study. This further demonstrates that PSWs and GUs are connected, and indicates that PSWs differ from Ps6 waves which have a similar wave period and irregular waveform but mainly concentrate in the dawnside and connect with Ω bands. PSWs preferentially occur under the condition of high solar wind velocities (VSW > 500 km/s) and high dynamic pressures (Pdyn > 5 nPa), and their occurrence rate has a negative correlation with IMF Bz, SYMH and AL. Statistical results also reveal that PSWs preferentially occur around the peak of both magnetic storms and substorms. These findings may shed new lights on the further understanding of PSWs' generation and propagation.

How to cite: Feng, Z.-J., Ren, J., Zong, Q.-G., Xiang, T.-Y., and Ai, X.-Y.: Statistical Properties of Long-Period Plasmapause SurfaceWaves From Van Allen Probes Observations, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-7559, https://doi.org/10.5194/egusphere-egu24-7559, 2024.