Pitch-angle diffusion is one of the main processes of isotropisation of ions in the Earth's magnetosheath. It results from the proton cyclotron and mirror instabilities, arising from temperature anisotropy in the magnetosheath, and is governed by the pitch-angle diffusion coefficient D_μμ. We have previously developed a sub-grid model to describe pitch-angle diffusion in global-hybrid Vlasov simulations when coarse spatial grid resolution leads to a lack of diffusion. In this study, we present an analytical solution for a pitch-angle diffusion coefficient derived from bi-Maxwellian velocity distribution functions in order to apply this solution to the sub-grid model. This will allow us to model accurately the isotropisation of the distribution functions and to reduce the temperature anisotropy of the plasma while saving computational resources. 

How to cite: Dubart, M., Battarbee, M., Ganse, U., Osmane, A., Spanier, F., Alho, M., Cozzani, G., Bussov, M., Horaites, K., Pfau-Kempf, Y., Suni, J., Tarvus, V., Turc, L., Zaitsev, I., Zhou, H., and Palmroth, M.: Determination of pitch-angle diffusion coefficient from bi-Maxwellian velocity distribution functions, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-6680, https://doi.org/10.5194/egusphere-egu23-6680, 2023.

A high-precision model of steady-state plasma flow and magnetic field in the planetary magnetosheath region is proposed by introducing the concept of conformal mapping and transforming the Kobel-Flueckiger scalar potential (the exact solution of Laplace equation) from the parabolic boundaries (bow shock and magnetopause) into arbitrary shape of boundaries. While the statistically-confirmed bow shock and magnetopause models can often be extended to the complex plane by analytic contiuation, construction of conformal mapping in a general magnetosheath case turns out be a mathematical challenge. The reason for this is that the analytic continuation of the bow shock shape does not necessarily meet the analytic contination of the magnetopause shape in general. We overcome this problem and construct a numerical conformal mapping method for the magnetosheath with arbitrary bow shock and magnetopause shapes by (1) modeling shell-like envelopes that smoothly change vary between the two boundaries (the v-variables), (2) imposing the orthogonality condition to find normal directions to the envelopes (the u-variables), and (3) applying the u and v variables to the Kobel-Flueckiger potential. Our conformal mapping method serves as a reference model of magnetosheath, which is numerically inexpensive and is easily implemented. Analysis of in-situ measurement data and numerical simulations of the planetary magnetosheath region will significantly benefit from the conformal mapping method. Moreover, our method can be used to derive the upstream conditions (flow speed and magnetic field) using the magnetosheath data.

How to cite: Narita, Y., Toepfer, S., and Schmid, D.: Conformally-mapped planetary magnetosheath model, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-9280, https://doi.org/10.5194/egusphere-egu23-9280, 2023.

Global magnetohydrodynamic models predict that plasma velocities vary almost linearly from 0 km s^-1 at the stationary subsolar magnetopause to ~0.25 V_SW at the subsolar bow shock, where V_SW is the solar wind velocity.  We show how two-point measurements of the plasma velocity  within ~15° of the Sun-Earth line can be used to determine gradients in the plasma velocity and consequently the time-dependent location of both the subsolar magnetopause and the subsolar bow shock.  A case study employing multiple simultaneous THEMIS spacecraft observations confirms that velocity gradients in the subsolar magnetosheath are linear, except when spacecraft observe rapid fluctuations downstream from the quasi-parallel bow shock.  The method may be useful to those binning magnetosheath observations to develop empirical models, those seeking to determine whether reconnection and hence magnetopause erosion are steady or bursty, and those determining the stand-off distance of the bow shock (or equivalently the polytropic index in the solar wind).

How to cite: Sibeck, D. and Silveira, M.: Tracking the Subsolar Bow Shock and Magnetopause, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-2460, https://doi.org/10.5194/egusphere-egu23-2460, 2023.

The solar wind prediction in front of the Earth relies on the spacecraft observations at the L1 point. In the last decade, the Wind and ACE missions orbiting around the L1 point were accompanied with the DSCOVR spacecraft. This configuration allows determination of the spatial structure of solar wind discontinuities that in turn impact the Earth. Processes in the heliospheric current sheet can produce structures with scales comparable to the entire dayside magnetosphere and such structures can be misinterpreted using OMNI data that are based on observations in one point only. In this study, we present the tracing of such inhomogeneous structures in the solar wind from L1 toward the Earth. We analyze in details their manifestation in the magnetosheath, at the magnetopause and inside the magnetosphere with motivation to more precisely determine the shape and location of magnetospheric boundaries. Moreover, we investigate the mechanisms leading to creation and development of such structures in the solar wind.

How to cite: Grygorov, K., Němeček, Z., and Šafránková, J.: Non-uniform structures in the solar wind and its interaction with the Earth’s magnetosphere, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-3157, https://doi.org/10.5194/egusphere-egu23-3157, 2023.

The Solar wind Magnetosphere Ionosphere Link Explorer (SMILE) is a Chinese Academy of Science (CAS) and European Space Agency (ESA) collaborative science mission. Primary goals are investigating the dynamic response of the Earth’s magnetosphere to the solar wind (SW) impact via simultaneous in situ SW/magnetosheath plasma and magnetic field measurements, X-Ray images of the magnetosheath and magnetic cusps, and UV images of global auroral distributions.  Recently, soft X-ray emissions from SW charge exchange (SWCX) at Earth’s magnetosphere has been investigated using XMM-Newton observations (Zhang et al., ApJL, 2022). Their results reveal that heavy ions (e.g., O⁷⁺) have relatively discrete and intense spectral lines, which can be more easily captured by soft-X ray instrument. Another striking point is that the fitted X-ray flux emitted by the ion line is sensitive and correlated to some physical values of SW bulk speed and density. To obtain physical quantities self-consistently for SW heavy ions, a three-dimensional global hybrid model has been developing. Based on Zoltan, ParGrid, and Corsair, we have developing a three-dimensional hybrid model of the terrestrial magnetosphere combining several modules: e.g., open boundaries with different particle injectors, cold plasma model for the inner magnetosphere, magnetosphere-ionosphere coupling module, and vtk format IO etc. In this poster, we will present preliminary results on the global dynamics of proton and heavy ions from the Earth’s bow shock all the way to the magnetopause under quasi-radial IMF conditions. This research focuses on 3-D profiles of key physical parameters, such as the magnetosheath ion pressure and high speed jets. And the resulting deformation of the magnetopause also will be discussed. Heavy ion behaviors at above dynamic/kinetic structures may play important roles in their soft X-ray emission during the interaction between SW heavy ions and the Earth’s exosphere (mainly populated by neutral hydrogen atoms). Thence, we will represent and compare the soft-X ray imaging calculated by heavy-ion data and proton data, respectively.

How to cite: Yang, Z., Guo, X., Sun, T., Jarvinen, R., Parks, G. K., Huang, C., Li, H., and Wang, C.: Deformations at Earth's dayside magnetopause under quasi-radial IMF: implications for the SMILE soft X-ray imaging, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-1110, https://doi.org/10.5194/egusphere-egu23-1110, 2023.

The Lunar Environment Heliospheric X-ray Imager (LEXI, lunar flatform) and Solar wind-Magnetosphere-Ionosphere Link Explorer (SMILE, high apogee Earth-orbiter) will take photos of the Earth’s dayside magnetopause and cusps in soft X-rays after their respective launch in 2024 and 2025 for understanding global magnetic reconnection modes under varying solar wind conditions. To support successful science closure, it is critical to develop techniques to extract magnetopause position from observed soft X-ray images. In this presentation, we introduce a new method that derives subsolar magnetopause position (SMP) as a function of a satellite location and a look direction that gives peak soft X-ray emission. Two assumptions are used in this method: 1. The look direction of maximum soft X-ray emission is the tangent to magnetopause, 2. the magnetopause near a subsolar point is nearly spherical and thus the SMP is equal to the radius of magnetopause curvature. We test this magnetopause tracing method by using the anticipated LEXI soft X-ray images under various solar wind conditions. First, we simulate synthetic soft X-ray images observed from various LEXI locations using the OpenGGCM global magnetosphere MHD model. Galactic background, particle background, and Poisson noises are considered in these images. Then, we apply a lowpass filter to the synthetic LEXI images for removing noises and obtaining accurate look angles of soft X-ray peaks. From filtered images, we calculate SMPs for various LEXI locations and solar wind fluxes, and estimate its accuracy by using the SMPs of OpenGGCM as ground truth. Our method estimates SMPs with an accuracy of <0.3RE and this accuracy improves as the solar wind density increases.

How to cite: Kim, H., Connor, H., Jung, J., Walsh, B., and Sibeck, D.: Estimating the Subsolar Magnetopause Position from Soft X-ray Images using Lowpass Image Filter, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-9761, https://doi.org/10.5194/egusphere-egu23-9761, 2023.

The interaction between the solar wind and the Earth's magnetosphere, and the geospace dynamics that result, is one of the key questions in space plasma physics. In situ instruments on a fleet of solar wind and magnetospheric constellation missions now provide the most detailed observations of Sun-Earth connections over multiple scales, from the smallest of a few kilometres up to the largest of a few 10s of Earth radii. However, we are still unable to quantify the global effects of the drivers of such connections, including the conditions that prevail throughout geospace. This information is the key missing link for developing a complete understanding of how the Sun gives rise to and controls Earth's plasma environment and space weather. This is where SMILE (Solar wind Magnetosphere Ionosphere Link Explorer) comes in.
SMILE is a novel self-standing mission dedicated to observing the solar wind - magnetosphere coupling via simultaneous in situ solar wind/magnetosheath plasma and magnetic field measurements, soft X-ray imaging of the magnetosheath, magnetopause and polar cusps, and UV imaging of the northern hemisphere auroral oval. Remote sensing of the magnetosheath and cusps with soft X-ray imaging is made possible thanks to solar wind charge exchange (SWCX) X-ray emissions known to occur in the vicinity of the Earth's magnetosphere. SMILE is a joint mission between ESA and the Chinese Academy of Sciences (CAS) due for launch at the beginning of 2025. SMILE science objectives as well as the latest scientific and technical developments jointly undertaken by ESA and CAS and the international instrument teams will be presented.

How to cite: Escoubet, C.-P., Branduardi-Raymont, G., and Wang, C. and the SMILE team: SMILE: a mission to image the solar wind-magnetosphere interaction, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-12353, https://doi.org/10.5194/egusphere-egu23-12353, 2023.

In this study, a new analytical model to describe the time-dependent subsolar magnetopause motion under interplanetary magnetic field (IMF) southward turning has been developed. This model, based on the scenario of magnetopause erosion due to magnetic reconnection, can be approximated by both linear and non-linear functions. The linear function is simplified under the assumption of constant magnetopause erosion under southward IMF, and the non-linear function is derived by assuming that the magnetopause erosion decays exponentially. In the limit of a short time, the non-linear function is essentially the same as the linear function. By comparing with global MHD simulations, the linear function performs well within the first ten minutes, and the error then increases with time. The non-linear function describes the magnetopause motion more accurately with respect to, and consistent with simulations for a time interval of $\sim 40$ minutes. This model has also been successfully applied to data-driven simulations of the 17 March 2015 geomagnetic storm event, suggesting the possible applicability of this model in reality. 

How to cite: Xu, Q., Tang, B., Sun, T., Zhang, X., Wei, F., Guo, X., and Wang, C.: Modeling of the Subsolar Magnetopause Motion Under Interplanetary Magnetic Field Southward Turning, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-10542, https://doi.org/10.5194/egusphere-egu23-10542, 2023.

The Kelvin-Helmholtz Instability (KHI) plays a significant role in the viscous-like mass, momentum, and energy transfer from the solar wind into the magnetosphere through both vortical and wave dynamics. To confidently study and compare the effects of these dynamics, we must formally define a vortex. Previously, a definition did not exist for the magnetohydrodynamic (MHD) regime. Consequently, we have developed a novel vortex definition (the `λ_MHD definition’) for MHD flows. This is based on adapting well-used hydrodynamic techniques (the λ₂ family of methods) that defines a vortex as a local minimum in an adapted pressure field. We derive the MHD suitable adapted pressure field from the ideal MHD Cauchy-Momentum equation, and find that it is composed of four components. The first three components represent the hydrodynamic properties of rotational momentum flow, density inhomogeneity, and fluid compressibility respectively. The final component makes the λ_MHD definition unique from hydrodynamics as it represents the rotational component of the J×B Lorentz force which is found using a Helmholtz decomposition. We use the Gorgon global 3-Dimensional MHD code to validate the λ_MHD vortex definition within a northward IMF simulation run exhibiting KHI-driven waves at the magnetopause flanks. Comparison of λ_MHD with existing hydrodynamic definitions shows good correlations and skill scores, particularly with the more advanced methods. Our analysis also reveals that the rotational momentum flow term dominates at the magnetopause. The other components provide typically small corrections to this. We have found that at the magnetopause, compressibility generally acts in opposition to the existence of a pressure minimum and thus a vortex. Alternatively, inhomogeneity and the rotational component of the Lorentz force generally act to support the pressure minimum. We explore potential physical reasons for these results and discuss potential applications of this method to further simulation and spacecraft observations.

How to cite: Kelly, H., Archer, M., Eggington, J., Heyns, M., Southwood, D., Desai, R., Eastwood, J., Mejnertsen, L., and Chittenden, J.: Formation and identification of Kelvin-Helmholtz generated vortices at Earths magnetopause: Insight from adapting hydrodynamic techniques for MHD, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-6613, https://doi.org/10.5194/egusphere-egu23-6613, 2023.

Increases in the solar wind dynamic pressure compress the magnetosphere, enhance magnetic field strengths and push the magnetopause inward.  Enhanced reconnection on the magnetopause, as might be expected during southward IMF conditions, launches rarefaction waves into the magnetosphere, decreases magnetic field strengths, and erodes the magnetopause inward.  Nightside magnetotail magnetic fields stretch tailward during erosion events and ultimately snap back to dipolar orientations at substorm onset.  The effects can be seen clearly in geosynchronous orbit.  We present a statistical survey of the effects of magnetopause motion and substorm stretching and dipolarization on magnetic fields deep inside both the dayside and nightside magnetosphere using observations from NOAA’s GOES satellites.

How to cite: Hsieh, S.-Y. and Sibeck, D.: The Effects of Magnetopause Motion and Substorm Stretching and Dipolarization on Magnetic Fields in the Inner Magnetosphere , EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-10776, https://doi.org/10.5194/egusphere-egu23-10776, 2023.

 In this study, we reported the large‐amplitude and fast‐damped flapping of the plasma sheet,
which co‐occurred with magnetic reconnection. Data from the Double Star TC‐1 and Cluster satellites
were used to analyze the features of the plasma sheet flapping 1.4 RE earthward of an ongoing magnetic
reconnection event. The flapping was rapidly damped, and its amplitude decreased from the
magnetohydrodynamics scale to the subion scale in 5 min. The variation in the flapping period (from 224 to
20 s) indicated that the source of the flapping had highly dynamic temporal characteristics. The plasma sheet
flapping propagated duskward through a kink‐like wave with a velocity of 100 km/s, which was in
agreement with the group velocity of the ballooning perturbation. A correlation analysis between the
magnetic reconnection and plasma sheet flapping indicated that the magnetic reconnection likely facilitated
the occurrence of ballooning instability by altering the state of plasma in the downstream plasma sheet. In
this regard, the reconnection‐induced ballooning instability could be a potential mechanism to generate
the flapping motion of the plasma sheet. 

How to cite: Zhang, Y., Dai, L., Rong, Z., Wang, C., Reme, H., Dandouras, I., Carr, C., and Escoubet, P.: Observation of the Large‐Amplitude andFast‐Damped Plasma Sheet FlappingTriggered by Reconnection‐InducedBallooning Instability, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-1047, https://doi.org/10.5194/egusphere-egu23-1047, 2023.

The near-Earth electromagnetic environment represents a far-from-equilibrium system. The magnetosphere exhibits nonstationary and nonlinear dynamics, especially during magnetic storms. For a broad class of complex phenomena, the dynamics can be interpreted in terms of a superposition of stochastic and deterministic components, occurring at different time scales. The main feature of a magnetic storm is the depression of the horizontal magnetic field component at low latitudes due to the enhancement of the ring current activity. In this work we use the SYM-H geomagnetic index, which is meant for monitoring the global variation of the horizontal component of the Earth’s magnetic field along the equator. The aim of this work is to model the SYM-H dynamics via stochastic differential equations whose parameters are properly retained from data. As a first step we investigate the Markovian character of SYM-H, which accurately satisfies this requirement with 1-min time resolution. This allows us to model the SYM-H dynamics via Kramers–Moyal analysis. We give evidence that a purely diffusive process is not representative of the observed dynamics and then a model based on jump-diffusion processes must be taken into account in order to reproduce correctly the dynamical features of the SYM-H index. In light of recent findings on auroral electrojet dynamics, high-latitude magnetospheric activity also shows a jump-diffusion character on small time scales. A discussion of the future perspective of a comprehensive model of both auroral activity and ring current dynamics based on the multivariate Kramers-Moyal analysis is addressed.

* This research has been carried out in the framework of the CAESAR project, supported by the Italian Space Agency and the National Institute of Astrophysics through the ASI-INAF n. 2020-35-HH.0 agreement for the development of the ASPIS prototype of scientific data centre for Space Weather.

How to cite: Benella, S., Consolini, G., Stumpo, M., and Alberti, T.: A semi-empirical model for magnetic storm dynamics, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-7165, https://doi.org/10.5194/egusphere-egu23-7165, 2023.

Magnetospheric sawtooth events (STE) are periodic oscillations in Earth’s magnetic field and energetic particle fluxes, typically occurring during geomagnetic storms. While previous studies have helped to provide information about the characteristics of STEs and the conditions that lead to the onset of these events, very little research has been done in the past 10 years documenting STEs, and analyzing the inner magnetosphere magnetic configuration during sawtooth events. This information can help understand how storms and substorms affect ionosphere-thermosphere convection, and how low-latitude ionospheric disturbances are generated during substorms. This project uses observations from magnetospheric missions and ground-based magnetometer networks to study the sawtooth event processes. Using magnetic field measurements GOES and the auroral electrojet indices, we are able to identify and catalog sawtooth events. We present our methods for identifying sawtooth events and preliminary statistics of the event characteristics. Then using magnetic field measurements from the THEMIS, RBSP, and MMS missions, we will study the evolution of the ring current and its latitudinal and longitudinal variations during STEs. We will also assess the abilities of the empirical Tsyganenko field models to reproduce the magnetospheric conditions during sawtooth events.

How to cite: DiMarco, C., Pulkkinen, T., Kumar, S., and Ala-Lahti, M.: Statistics of Magnetospheric Sawtooth Oscillations, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-9233, https://doi.org/10.5194/egusphere-egu23-9233, 2023.

With the increased availability of ground magnetic field measurements from the Northern and Southern hemispheres at higher latitudes, further insight could be gained into how the physical processes coupling magnetosphere and ionosphere vary with solar wind forcing. In this study, we report a solar wind dynamic pressure enhancement followed by an interplanetary magnetic field clock angle change on February 13, 2014. We use measurements from East Antarctica and West Greenland regions to investigate when and where the magnetic field signatures differ. Finally, we use the University of Michigan Space Weather Framework (SWMF) to conduct numerical simulations to explain the differences in the interhemispheric responses to the changes in solar wind dynamic pressure enhancement and IMF clock angle together and separately. 

This work is supported by NASA LWS Program and makes use of the NASA High-End Computing Capability.

How to cite: Ozturk, D., Kim, H., Xu, Z., and Kuzichev, I.: Untangling the Interhemispheric Response to Solar Wind Drivers through Numerical Experiments, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-7628, https://doi.org/10.5194/egusphere-egu23-7628, 2023.

We present simulation results of a transpolar auroral arc event that show the arc formation occurs on both open and closed field lines and is sourced from both dayside and nightside magnetospheric reconnection. The dayside and nightside precipitation sources magnetically connect across the polar cap in a flow channel to create the transpolar arc structure. We simulate the 15 May 2005 transpolar arc event observed by the IMAGE satellite with the University of Michigan Space Weather Modeling Framework (SWMF) Geospace configuration. We compare the IMAGE observations to the simulation produced ionospheric Joule heating to identify the transpolar arc features captured by the model. The features exist within an anti-sunward flow structure and coincide with the location of the R1/R2 current reversal. We map the magnetic field lines from the arc features to the magnetosphere, revealing both dayside and nightside source regions. We use four-field junction analysis to determine that the source regions are within potential simulation reconnection sites. We simulate other transpolar auroral arcs to assess the generality of our results.

How to cite: Hill, S., Pulkkinen, T., Brenner, A., Al Shidi, Q., Mukhopadhyay, A., Kullen, A., Frey, H., Zou, S., and Liemohn, M.: The Magnetospheric Source of Theta Aurora Include Dayside and Nightside Multiple Reconnection Sites: SWMF Geospace Simulation Results, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-11389, https://doi.org/10.5194/egusphere-egu23-11389, 2023.

We have recently discovered a new auroral structure called "auroral dripping" with ground-based and magnetospheric conjugated observations. They are frequent drippings from higher latitudes toward the equator, with a duration of 10-20 minutes. Magnetospheric observations show increases in particle flux and magnetic field simultaneously. With the keograms and ewograms, we find that the auroral drippings are different from other periodic structures in the motion and the temporal periodicity. To investigate the possible magnetospheric source of this structure, we simulate the entire process with the Rice Convection Model coupled with an MHD code (RCM-MHD). After long-lasting low-entropy plasma is supplied from the tailward boundary, frequent drippings and the accompanying oscillations in the near-Earth plasma sheet are reproduced. Our preliminary results suggest that the continuous plasma injection is considered to be possible magnetospheric source of the auroral dripping.

How to cite: Wang, W., Yang, J., and Zhang, F.: Auroral dripping and its possible magnetospheric source, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-11674, https://doi.org/10.5194/egusphere-egu23-11674, 2023.

We review the range of applications and use of the curlometer, initially developed to analyze electric current density using Cluster multi-spacecraft magnetic field data; but more recently adapted to other arrays of spacecraft flying in formation, such as MMS small-scale, 4-spacecraft configurations; THEMIS close constellations of 3-5 spacecraft, and Swarm 2-3 spacecraft configurations. The method (and associated methods based on spatial gradients) has been shown to be easily adaptable to other multi-point and multi-scale arrays. Although magnetic gradients require knowledge of spacecraft separations and the magnetic field, the structure of the electric current density (for example, its relative spatial scale), and any temporal evolution, limits measurement accuracy. Nevertheless, in many magnetospheric regions the curlometer is reliable (within certain limits), particularly under conditions of time stationarity, or with supporting information on morphology (for example, when the geometry of the large scale structure is expected). A number of large-scale regions have been investigated directly, such as: the cross-tail current sheet, ring current, the current layer at the magnetopause and field-aligned currents. In addition, the analysis can support investigations of transient and smaller scale current structures (e.g. reconnected flux tubes, boundary layer sub-structure, or dipolarisation fronts) and energy transfer processes. The method is able to provide estimates of single components of the vector current density, even if there are only two or three satellites flying in formation, within the current region, as can be the case when there is a highly irregular spacecraft configuration. The computation of magnetic field gradients and topology in general includes magnetic rotation analysis and various least squares approaches, as well as the curlometer, and indeed the combination with plasma measurements and the extension to larger arrays of spacecraft have recently been considered. We touch on these extensions and on new methodology accessing the properties of the underlying formulism.

How to cite: Dong, X., Dunlop, M., Shen, C., Wang, T., Robert, P., Eastwood, J., Haaland, S., Yang, Y., Tan, X., Escoubet, P., Rong, Z., Fu, H., and De Keyser, J.: Curlometer technique and applications, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-13116, https://doi.org/10.5194/egusphere-egu23-13116, 2023.

The SCIentific Qt application for Learning from Observations of Plasmas (SciQLop) project allows to easily discover, retrieve, plot and label in situ space physic measurements stored on remote servers such as Coordinated Data Analysis Web (CDAWeb) or Automated Multi-Dataset Analysis (AMDA).  Analyzing data from a single instrument on a given mission can raise some technical difficulties such as finding where to get them, how to get them and sometimes how to read them.  Thus building for example a machine-learning pipeline involving multiple instruments and even multiple spacecraft missions can be very challenging. Our goal here is to remove all these technical difficulties without sacrificing performances to allow scientist to focus on data analysis.

The SciQLop project is composed of the following tools:

• Speasy: An easy to use Python package to retrieve data from remote servers with multi-layer cache support.
• Speasy_proxy: A self-hostable, chainable remote cache for Speasy written as a simple Python package.
• Broni: A Python package which finds intersections between spacecraft trajectories and simple shapes or physical models such as magnetosheath.
• Orbit-viewer: A Python graphical user interface (GUI) for Broni.
• TSCat: A Python package used as backend for catalogs of events storage.
• TSCat-GUI: A Python graphical user interface (GUI).
• SciQLop-GUI: An extensible and efficient user interface to visualize and label time-series with an embedded IPYthon terminal.

While some components are production ready and already used for science, SciQLop is still in development and the landscape is moving quite fast.

In this poster we will demonstrate how the SciQLop project makes masive in-situ data analysis simple and fast and we will also take the oportunity to exchange ideas with our users.

How to cite: Jeandet, A., Aunai, N., Génot, V., Boettcher, P., Renard, B., Michotte de Welle, B., André, N., Bouchemit, M., and Dufourg, N.: SciQLop:  a tool suite to facilitate multi-mission data browsing and analysis, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-13581, https://doi.org/10.5194/egusphere-egu23-13581, 2023.

In the solar wind density, we often observe periodic fluctuations on time scales ranging from a few minutes to a few hours which we refer to as Periodic Density Structures (PDSs). The PDSs belong to the class of “meso-scale structures” with radial length scales greater than or equal to the size of the Earth’s dayside magnetosphere. The periodic character of these transients (≈0.2-4.0 mHz) can determine periodic compressional fluctuations of the Earth’s magnetic field at similar frequencies (“forced breathing” mode). The corresponding time scales overlap with the frequency range of Pc5 Ultra Low Frequency (ULF) waves (≈1.7-6.7 mHz). The compressional “forced breathing” fluctuations are often global and impact the entire Earth’s magnetosphere system/dynamics.  Using a recently developed spectral analysis approach applied to magnetic field observations at satellites and ground stations, we were able to differentiate directly driven magnetic field oscillations from Pc5 ULF waves triggered by other sources. Here, we discuss clear examples of such a directly driven process also showing effects on radiation belt electron dynamics and loss.

How to cite: Di Matteo, S., Kepko, L., Viall, N., Breneman, A., Halford, A., and Villante, U.: Earth’s magnetosphere dynamics during “forced breathing” due to solar wind periodic density structures, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-10258, https://doi.org/10.5194/egusphere-egu23-10258, 2023.

Magnetospheric substorm is recognized as an important mechanism for transferring and dissipating solar wind energy to the ionosphere and near-Earth regions. A substorm is generally thought to consist of three phases: growth phase, expansion phase, and the recovery phase, and the total duration of a substorm is about 2–4 hour. In this work, we present a statistical study of the magnetotail state during different phases of substorms, recovery phase in particular, for a period of 5 years from 2016-2020 using multi-spacecraft and ground magnetic measurements. For best spatial and temporal coverage of the inner magnetosphere and magnetotail, we use THEMIS, RBSP, MMS mission observations complemented by the SuperMAG database of measurements from ground-based magnetometers. To examine the duration of substorm expansion and recovery phases in the ionosphere, inner magnetosphere and magnetotail, we first find the substorm peak and end times from a list of substorm onsets available on the SuperMAG website. Substorm peak corresponds to the peak intensity of the westward electrojet provided by the SML (SuperMAG AL) index. For the current analysis period, we obtain a few thousand events when there are at least two spacecraft in the tail, which provides good statistics. To determine the time scales of expansion and recovery phases in the inner magnetosphere and magnetotail, we divide the observations into different bins based on X and Y position of the spacecraft. Keeping focus at the center of the tail, i. e., -5 < Y < 8 RE, the bins are chosen to be -4 to -7 RE, -7 to -10 RE, -10 to -15 RE, and -15 to -25 RE. A superposed epoch analysis is performed on the IGRF field subtracted ($ \Delta Bz =Bz_{Measured}- Bz_{IGRF}$) $Bz$ component of observed magnetic field for complete period of analysis. To find the time scale for recovery phase, we center the superposed epoch around the peak time. Our results show that the timescale of the field recovery is  more than an hour near the geostationary orbit (-4 to -7 RE), 30 min to less than an hour in the range -7 to -10 RE and even shorter as we go beyond -10 RE. The results presented in this work will help understand the spatial and temporal evolution of substorms in the magnetotail, and will significantly improve our understanding of space physics.

How to cite: Kumar, S., Pulkkinen, T., Connor, D., and Brenner, A.: Statistical study of substorm recovery phases  in the inner magnetosphere and magnetotail, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-3960, https://doi.org/10.5194/egusphere-egu23-3960, 2023.