In addition, the ESA Scout NanoMagSat constellation, consisting of one near-polar and two 60° inclination satellites, is scheduled to launch near the end of 2027, with full operation planned for 2028. It will acquire high-accuracy magnetic vector and scalar data, electron density, and electron temperature
data, navigation data, and collect ionospheric radio-occultation profiles. All these data are also complemented by increasingly available platform-magnetometer data, such as from the CryoSat-2, GRACE, GRACE-FO, GOCE, and E-POP satellites. The new abundance of satellite data provides unprecedented space-time data coverage at LEO satellite altitudes, opening the way for new scientific opportunities.
Orals: Tue, 5 May, 14:00–15:45 | Room -2.20
Geomagnetic field and ionospheric environment LEO monitoring is presently achieved by the three polar orbiting, two side-by-side and one with relative local time (LT) drift, satellites of the Swarm Earth Explorer ESA constellation launched in November 2013, forming the backbone of a broader constellation now also including the Chinese CSES-1 and CSES-2 missions launched in February 2018 and June 2025, maintained 180° apart on the same Sun-Synchronous orbit, as well as the Chinese MSS-1 41° inclination mission, launched in May 2023. These are currently the only missions carrying an absolute magnetometry payload critical for global field monitoring.
Here, we will present the latest status of the NanoMagSat constellation mission, third small science mission selected for ESA’s new Earth Observation fast track Scout program that taps into New Space. Scout is a new framework (3 years for implementation, cost ≤ 35 M€) by which ESA aims to demonstrate disruptive sensing techniques or incremental science, while retaining the potential to be subsequently scaled up in larger missions or implemented in future ESA Earth Observation programs.
NanoMagSat will cover all LT at all latitudes, with special emphasis on latitudes between 60°N and 60°S, where all LT will be visited within about a month, much faster than is currently achieved. Each 16 U satellite will carry an advanced miniaturized absolute scalar and self-calibrated vector magnetometer with star trackers collocated on an ultra-stable optical bench at the tip of a 3m deployable boom, a compact High Frequency Magnetometer at mid-boom, a multi-Needle Langmuir Probe and dual frequency GNSS receivers on the satellite body. This payload suite will acquire high-precision/resolution oriented absolute vector magnetic data at 1 Hz, very low noise scalar and vector magnetic field data at 2 kHz, electron density data at 2 kHz, and electron temperature data at 1 Hz. GNSS receivers will also allow recovery of top-side TEC and ionospheric radio-occultation profiles. NanoMagSat will start deploying in 2027, with full constellation to be operated for a minimum of three years between 2028 and 2031.
Science objectives will be introduced and the rationale for the choice of the payload and constellation design explained. The planned data products, with their expected performance, will also be described. Special emphasis will be put on the innovative aspects of the mission with respect to previous missions. Finally, possibilities of further expanding the constellation though international collaboration as encouraged by IAGA resolution 2025 n°1 will be discussed.
How to cite: Hulot, G., Coïsson, P., Léger, J.-M., Clausen, L. B. N., Jørgensen, J. L., van den Ijssel, J., Chauvet, L., Deborde, R., Salinas, M., Fillion, M., Troncy, S., Jager, T., Stoltze, C. B., Deconinck, F., Nieto, P., Cipriani, F., Pastena, M., and Lejault, J.-P.: The ESA Scout NanoMagSat Mission, a Nanosatellite Constellation to Further Improve Geomagnetic Field and Ionospheric Environment Monitoring and Modeling, on Course for First Launch in 2027, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-2836, https://doi.org/10.5194/egusphere-egu26-2836, 2026.
The Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites (TRACERS) is a recently launched NASA mission focused on investigating how temporal or spatial variations in magnetic reconnection drive cusp dynamics by employing multipoint, high-cadence measurements from two identical spacecraft. TRACERS successfully launched into a Sun-synchronous 590 km orbit around Earth on July 23, 2025. The two spacecraft comprising TRACERS are equipped with identical instrument payloads capable of measuring ions, electrons, and electromagnetic fields within low-Earth orbit. The primary goal of the TRACERS mission is to disentangle temporal and spatial variation of magnetic reconnection and associated processes by employing multipoint measurements within the cusp from two identical spacecraft (TRACERS-1 and -2), which are separated by 10 to 120 seconds. In addition to its primary science goals of examining cusp dynamics, TRACERS is also capable of measuring auroral precipitation and processes with high spatial and temporal resolution. We present initial auroral electron observations from one of the TRACERS spacecraft on October 7, 2025. We observe both discrete and diffuse electron precipitation in two orbits in the northern hemisphere. TRACERS-2 observes numerous inverted-V structures indicative of discrete aurora within the auroral oval and polar cap, as well as within the northern cusp. Hours later, TRACERS-2 observes broadband, diffuse electron precipitation spanning tens of eV to tens of keV across the northern polar cap, indicative of polar rain. We discuss the upstream solar wind conditions during each observation utilizing Wind data, as well as the characteristic energies, pitch angle distributions, and fluxes of each electron population observed by TRACERS-2 during these two observations.
How to cite: Henderson, S., Halekas, J., Strangeway, R., Bounds, S., Christopher, I., Moore, A., Ruhunsuri, S., and Miles, D.: Initial TRACERS Observations of Auroral Electron Precipitation: Case Studies of Diffuse and Discrete Aurora, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-6038, https://doi.org/10.5194/egusphere-egu26-6038, 2026.
EZIE, the Electrojet Zeeman Imaging Explorer, is a NASA three-Cubesat Heliophysics mission launch on March, 14, 2025. It employs four downward and cross-track looking miniaturized radiometers on each of the 6U CubeSat, flying in a pearls-on-a-string managed formation, to measure, for the first time, the two-dimensional structure and the temporal evolution of the electrojets flowing at altitudes of ~100–130 km. The four identical radiometers simultaneously measure polarimetric radiances of the molecular oxygen thermal emission at 118 GHz and employs the Zeeman sensing technique to obtain the current-induced magnetic field vectors at ~80 km, an altitude region very close to the electrojet. This measurement technique allows for the remote sensing of the meso-scale structure of the electrojets at four different cross-track locations simultaneously at altitudes notoriously difficult to measure in situ. Differential drag maneuvers are used to manage satellite along-track temporal separation to within 2–10 minutes between adjacent satellite to record the electrojet temporal evolution without the need for on-board propulsion. The combination of the sensing technique, compact instrument and Cubesat technologies allow EZIE to cost-effectively obtain never-before “mesoscale” measurements needed to understand how the solar wind energies stored in the magnetosphere are transferred to the thermosphere and ionosphere. In this paper, we will present the current status of the EZIE mission and a summary of the measurement products and its latest results.
How to cite: Yee, J.-H., Swartz, W. H., Merkin, V., Mesquita, R., Mosavi-Hoyer, N., Wind-Kelly, R., Hoffman, M., and misra, S. and the NASA EZIE Mission Science Team: Status and Latest Results from NASA’s Electrojet Zeeman Imaging Explorer (EZIE) , EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-8389, https://doi.org/10.5194/egusphere-egu26-8389, 2026.
The University of Colorado Boulder is scheduled to launch the Compact Spaceborne Magnetic Observatory (COSMO), a 6U CubeSat mission at LEO designed to provide high-resolution measurements of the Earth's magnetic field in support of the next-generation World Magnetic Model (WMM), in March 2026. The payload, known as the Vectorize Rubidium Magnetometer (VRuM), is designed to be less than 1U in size and consists of two optical rubidium scalar magnetometers integrated within a triaxial Braunbek coil system and two star trackers. The Braunbek coils are stimulated with modulation currents at distinct frequencies to generate modulation magnetic fields along each axis, allowing for the vector extraction of the Earth’s magnetic field. In combination with the optical scalars and the Braunbek coil system, the VRuM instrument can be self-calibrated and can also measure the vector magnetic field. After the commissioning phase, in-orbit calibrations and tests will be performed. The in-orbit calibrations include vector calibration, heading error calibration, spacecraft bias characterization, and mounting quaternion determination. The vector calibration aims to determine the non-orthogonality of the coils and the magnitude of modulation fields. The heading error calibration characterizes the heading error of the scalars due to the non-alignment between the measured magnetic field and the cell within the scalars. The spacecraft bias test is designed to determine the static magnetic field created by the small amounts of magnetic material around the payload; this bias field has been estimated on the ground as less than 10 nT. The mounting quaternion is a parameter that transfers the coordinates between the coil system and the star trackers. To obtain the most accurate attitude information, the Uncented Kalman filter is applied. This paper outlines the mission design, magnetometer vectorization technique, calibration methods, and plans for in-orbit calibrations in combination with first observations from space.
How to cite: Kao, T.-H., Chism, C., Kaplan, O., Ellmeier, M., Knappe, S., Hughes, J., and Marshall, R.: In-Orbit Calibration of Vectorized Rubidium Magnetometer onboard COSMO, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-856, https://doi.org/10.5194/egusphere-egu26-856, 2026.
The Earth’s upper atmosphere is highly sensitive to solar activity and the solar wind-magnetosphere interaction. Magnetospheric current systems close through the ionosphere, where ion-neutral collisions and enhanced energetic particle precipitation can significantly modulate the spatial and temporal variability of the atmosphere's outer extent. Unlike the many isolated in-situ measurements conducted by previous space missions, distributed observations of neutral particles, plasma, and magnetic fields by a tetrahedron of micro-satellites, combined with precise tracking of satellite orbital dynamics, provide the global perspective needed to disentangle the complex transfers of energy and momentum through the tightly coupled magnetosphere-ionosphere-thermosphere system.
In this presentation, we outline the ROARS F3 mission architecture. This mission seeks to obtain the first full curlometer magnetic field and energetic particle precipitation measurements in low Earth orbit (LEO), alongside concurrent measurements of the ambient plasma and neutral populations across a range of altitudes, latitudes, and longitudes. The measurement strategy is designed to resolve and characterise the energy and momentum entering the upper atmosphere, the multi-scale pathways through which these are redistributed, and the feedback mechanisms coupling back to the broader geospace environment. A comprehensive ground segment will simultaneously provide context by relating information on D- and E-region dynamics to the in-situ measurements.
How to cite: Blake, J., Desai, R., Barabash, S., Burchill, J., Brown, M., Coxon, J., Daggitt, T., Dunlop, M., Fausch, R., Hnat, B., Hulot, G., Leger, J.-M., Lin, D., Nakamura, R., Nilsson, H., Panov, E., Radhakrishna, S., Vorburger, A., Walach, M., and Wang, X.-D.: ROARS: Research Observatory for Atmospheric Responses to Sun-magnetosphere interactions, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-13266, https://doi.org/10.5194/egusphere-egu26-13266, 2026.
This presentation provides an overview of the latest designs and development of the RADiation Impacts on Climate and Atmospheric Loss Satellite (RADICALS) mission, and which will launch in October 2027. The RADICALS is a Canadian small satellite mission with a payload designed to characterise energetic particle precipitation (EPP), to assess the physical mechanisms which cause it, and investigate the related impacts on the Earth’s atmosphere. EPP plays a critical role in altering atmospheric chemistry, particularly through the production of NOx and HOx, which catalytically destroy ozone in the middle atmosphere. The RADICALS will focus on measuring the energy input from precipitating energetic particles into the atmosphere, shedding new light on the connection between space weather and climate. Operating in a polar orbit, the RADICALS payload contains dual High Energy Particle Telescope (HEPT) suites (each comprising high and low energy telescopes, and a high temporal resolution scintillator), and dual X-Ray Imager (XRI) suites. When mounted on the spinning RADICALS spacecraft they will provide pitch angle distributions of trapped radiation belt electrons and solar energetic protons, twice per spin, as well as the associated Bremsstrahlung X-rays from atmospheric interactions. The mission's unique back-to-back HEPT suite design will measure both down-going and up-going particles simultaneously, while the XRI will remotely sense particle precipitation via X-ray emissions as well as monitoring lower energy electrons as a secondary product. The payload also includes a pair of boom-mounted fluxgate magnetometers and a 3-axis and search coil magnetometer to substantiate particle measurements with the local magnetic wave activity. By resolving the electron loss cone and quantifying the energy flux of precipitating particles, RADICALS will provide essential data for understanding how space radiation influences atmospheric chemistry, particularly during geomagnetic storms.
How to cite: Mann, I., Cully, C., Fedosejevs, R., Knudsen, S., Milling, D., Enno, G., Lipsett, M., Zee, R., Rankin, R., Connors, M., McWilliams, K., Ward, W., Fiori, R., Olifer, L., Ozeke, L., Marshall, R., Cullen, D., Barona, D., Howarth, A., and Yau, A.: Investigating Space Radiation and Atmospheric Climate Impacts with the Canadian RADICALS Mission, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-15926, https://doi.org/10.5194/egusphere-egu26-15926, 2026.
Continuous monitoring of electric current systems in Earth’s environment, including the ionosphere and magnetosphere, is essential for characterising geospace. Such observations are required, for example, to determine the energy input into the upper atmosphere and to monitor disturbances in the space environment and associated hazards. This monitoring can be achieved through magnetic field measurements acquired both on the ground and in space.
The spatio-temporal sampling provided by dedicated magnetic satellite missions such as Swarm and MSS can be significantly enhanced by incorporating platform magnetometer data from non-dedicated missions, including CryoSat-2, GRACE, and GRACE-FO.
This presentation reports recent achievements in the use of platform magnetometer data within a study funded by ESA’s General Support Technology Programme (GSTP). In particular, it highlights the calibration and provision of magnetic field data from ESA’s Aeolus satellite.
How to cite: Olsen, N., Cipriani, F., Iorfida, E., Thomsen, P. L., and Hansen, F.: Advanced Modelling of Geospace (AMOG) Using Satellite Platform Magnetometers, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-19387, https://doi.org/10.5194/egusphere-egu26-19387, 2026.
The growing constellation of low-Earth-orbit satellites allows us to characterize the thermosphere-ionosphere system (TI). One of the most valuable LEO measurements are accelerometer derived neutral density estimates, which play a central role in satellite drag estimations, TI modeling, and space weather operations. Despite their importance, the measurement uncertainty of satellite-derived neutral density for most LEO missions remains unknown. In this study, we use a data assimilation (DA) based framework to diagnose the observation uncertainty directly from neutral density measurements.
Using the Coupled Thermosphere Ionosphere Plasmasphere electrodynamics model (CTIPe) and TIDA, the TI Ensemble Kalman filter data assimilation scheme, we perform controlled experiments with varied assumed uncertainties. Two complementary diagnostics are applied: the Desroziers method, which estimates the effective observation uncertainty required for a self-consistent DA system, and an ensemble-spread method, which isolates the true measurement error by removing model-projected variability from the innovation variance.
We apply both diagnostics to CHAMP, Swarm A/B/C, and GRACE-A/B across low and high solar-activity periods. Results confirm the expected 10–15% uncertainty for CHAMP during quiet conditions, while GRACE (15–35%) and Swarm (25–50%) exhibit larger values, reflecting differences in altitude, solar activity, instrument characteristics, and thermospheric variability. The two methods provide complementary perspectives and the limit of the estimated uncertainty range: Desroziers quantifies the upper bound, and the ensemble-spread method provides the lower bound uncertainty. The framework provides a pathway to systematically quantify uncertainty in current and upcoming LEO missions, supporting improved density models, drag prediction, and space weather services.
How to cite: Fernandez-Gomez, I., Codrescu, S., Heymann, F., Borries, C., and Codrescu, M. V.: Diagnosing thermospheric density uncertainty from LEO satellites using data assimilation, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-1448, https://doi.org/10.5194/egusphere-egu26-1448, 2026.
Pc3-4 magnetic pulsations within the 16-100 mHz frequency range are mainly driven by the upstream waves (UWs) in the Earth’s foreshock region, which serves as a critical link for transferring energy from the solar wind into the magnetosphere-ionosphere system. High-precision magnetometer data from low Earth orbit (LEO) satellites, like CHAMP, Swarm and MSS-1, covering two solar cycles (from 2001-2025), provide a good database for resolving the characteristics of UWs. In this report, we performed a comprehensive analysis on UWs in the topside ionosphere, including their dependences on solar wind and interplanetary magnetic field conditions, season, magnetic local time, as well as latitude and longitudes. In addition, by analyzing the simultaneously measurements from these satellites with certain spatial separation, the propagation of UWs in the topside ionosphere has also been discussed.
How to cite: Xiong, C., Luehr, H., Xu, C., and Liu, H.: Compressional Pc3-4 magnetic pulsations in the topside ionosphere: observations from multiple LEO satellites, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-17072, https://doi.org/10.5194/egusphere-egu26-17072, 2026.
Mid-latitude semiannual noontime NmF2 peaks were analyzed at four Northern Hemisphere stations (Boulder, Rome, Wakkanai, Juliusruh) and two Southern Hemisphere stations (Hobart, Port Stanley). The aeronomic parameters responsible for the observed NmF2 variations were determined by solving an inverse problem of aeronomy using the original THERION method.
On average, the NmF2 peak in autumn is larger than the vernal peak in both hemispheres under solar minimum conditions. This observed difference in NmF2 between the two peaks is attributed to variations in thermospheric parameters that are not directly related to solar and geomagnetic activity. While the vernal peak can occur over a span of three months in both hemispheres, the autumnal peak is confined to a shorter two-month period.
The primary factor influencing the difference between NmF2 in the two peaks is the abundance of atomic oxygen [O]. A distinct two-hump NmF2 variation, with a trough in December–January in the Northern Hemisphere, reflects a lower concentration of [O] during this period compared to October–November. This variation is driven by changes in [O] rather than by the solar zenith angle effect.
The empirical MSISE00 model, which is based on observational data, suggests a global increase in total atomic oxygen abundance during the equinoxes. However, this increase cannot be explained by a simple redistribution of [O] within the thermosphere, as it represents a global-scale enhancement of atomic oxygen levels. The most plausible mechanism for controlling the global abundance of [O] in the thermosphere is the downward transfer of atomic oxygen via eddy diffusion.
At present, no alternative explanation sufficiently accounts for the global increase in total atomic oxygen during the equinoxes. This phenomenon remains a key area of interest in understanding the aeronomic processes governing thermospheric composition and its impact on ionospheric variability.
How to cite: Perrone, L. and Mikhaylov, A.: Equinoctial asymmetry in mid-latitude NmF2 noontime peaks: A formation mechanism , EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-7057, https://doi.org/10.5194/egusphere-egu26-7057, 2026.
The Earth’s ionosphere hosts a complex electric current system that generates magnetic fields. The study of these electric currents and fields provides crucial insights into the ionosphere-thermosphere system, lower atmospheric dynamics, magnetospheric physics, and ionospheric plasma distribution and dynamics.
A particularly valuable dataset to study these currents and fields comes from magnetic measurements acquired by low Earth orbit (LEO) satellites. Some of these satellites provide high-accuracy vector magnetic data that are calibrated using onboard independent scalar measurements. This is the case for the ESA Earth Explorer Swarm satellite constellation, the CHAMP satellite, or the more recently launched MSS-1 satellite. Other satellites, such as the GRACE, GRACE-FO, CryoSat-2, and GOCE satellites, provide complementary, less-accurate platform magnetic vector data, which help improve the overall space-time satellite data coverage. Data from all these satellites are already used to recover and study the signals from the Earth’s outer core, the lithosphere, the oceans, the magnetospheric and the E-region ionospheric currents, as well as the currents induced in the solid Earth by these time-varying ionospheric and magnetospheric fields.
Since LEO satellites orbit within the ionospheric F region, they also provide valuable in situ measurements of F-region ionospheric magnetic fields and electric currents. Interpreting the highly dynamic and spatially complex F-region signals in data from satellites at different altitudes and with very different geographic and local time coverage, however, is a challenging problem. A traditional approach in geomagnetism is to construct empirical models to extract and synthesize signals of interest from multiple data sources. Applied to F-region ionospheric fields and currents, it generally leads to strongly underdetermined inverse problems that can hardly be solved robustly due to incomplete satellite data coverage, even with modern satellite data. Recent research has nevertheless demonstrated that additional progress could be made by relying on optimized spatial basis functions using numerical simulations from realistic physics-based models, such as the Thermosphere-Ionosphere-Electrodynamics General Circulation Model. Such an approach has many advantages, including the ability to fill gaps at altitudes where no satellite data are available and to improve model numerical stability.
We will present our first very encouraging attempt to build a climatological model of F-region magnetic fields and ionospheric currents based on such an approach. Possible avenues for future improvements will also be discussed.
How to cite: Hulot, G., Fillion, M., Alken, P., Maute, A., and Egbert, G.: Physically constrained empirical modelling of climatological F-region magnetic field and electric current variations, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-7177, https://doi.org/10.5194/egusphere-egu26-7177, 2026.
High-precision magnetometry with absolute accuracy is crucial for monitoring the Earth’s magnetic field and advancing our understanding of core, lithospheric, and magnetospheric dynamics. Missions such as Ørsted, CHAMP (CHAllenging Minisatellite Payload), and ESA’s Swarm constellation have demonstrated the unique value of high-precision vector field and scalar magnetometer measurements carried out with absolute accuracy in Low Earth Orbit (LEO). Now imagine a world in which dedicated geomagnetic missions in LEO reach the end of their operational lifetimes, expected or otherwise, with no replacements in place. Without the insights provided by missions like Ørsted, CHAMP, and Swarm, we would lose a critical high-resolution view of Earth’s magnetic environment, leaving many variations unresolved. Moreover, data from dedicated magnetic missions are integral for calibrating platform magnetometers aboard satellites not designed for magnetic measurements. While such instruments remain operational, they lack the precision to capture fine-scale signals. Furthermore, without absolute-accuracy reference measurements, platform magnetometer data become less reliable, leading to increased inconsistencies across datasets.
Here, we examine the consequences of losing high-precision magnetometry with absolute accuracy in LEO for the calibration of platform magnetometers on satellites not dedicated to magnetic measurements. While reference geomagnetic information could still be derived from less accurate sources, such as ground-based observatory networks, these alternatives lack the spatial and temporal resolution uniquely provided by LEO observations and suffer from uneven global coverage, particularly over the oceans and other remote regions where observatories are sparse. Consequently, geomagnetic field models derived from such data would exhibit reduced resolution and accuracy, limiting their reliability and scientific scope. These deficiencies would propagate directly into the calibration of platform magnetometers, degrading their precision and consistency. This cascading effect would significantly impair our ability to monitor, understand, and model the dynamic geomagnetic field, including contributions from the core, lithosphere, and magnetosphere. Maintaining accurate, high-precision magnetometry in LEO is therefore essential to preserve the integrity of geomagnetic science and to support its wide range of scientific and practical applications.
How to cite: Kervalishvili, G., Schanner, M. A., Michaelis, I., Korte, M., Finlay, C., Kloss, C., Rother, M., Rauberg, J., and Qamili, E.: A World without Low Earth Orbit High-Precision Magnetometry: the next assessment, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-11045, https://doi.org/10.5194/egusphere-egu26-11045, 2026.
Substorms are transient, explosive events during which energy accumulated in the magnetosphere is rapidly released and dissipated in the high-latitude ionosphere. These events typically last 1–2 hours and may occur several times per day. Despite extensive observational and theoretical efforts, the physical processes governing substorm onset in the magnetosphere and the coupled ionospheric response remain incompletely understood. In particular, the spatiotemporal evolution of electrodynamic parameters during substorms and their dependence on solar wind driving require further investigation.
In this study, we integrate satellite and ground-based observations with the data assimilation technique, Local Mapping of Polar Ionospheric Electrodynamics (Lompe), to examine the global evolution of ionospheric electrodynamics during substorm events. Using Lompe, we reconstruct maps of ionospheric electric potential, ionosphere convection patterns, and field-aligned current systems, and analyze their temporal development throughout substorm phases. These parameters are analyzed in relation to the orientation of the interplanetary magnetic field (IMF). In addition, magnetospheric dynamics during substorms is inferred from estimates of the reconnection electric field, derived by calculating magnetic flux transfer across the open–closed field line boundary.
Our results provide a comprehensive global characterization of the polar ionospheric response to substorms and offer additional insights into the coupling between magnetospheric reconnection processes and ionospheric electrodynamics.
How to cite: Kebede, F., Laundal, K., Madelaire, M., and Hatch, S.: Substorm evolution as viewed from a data assimilation technique, Lompe., EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-11506, https://doi.org/10.5194/egusphere-egu26-11506, 2026.
ESA Earth Explorer Swarm mission, launched in November 2013 with the purpose of exploring and understanding the Earth’s interior and its environment, provided significant achievements in the observation of the geomagnetic field, the ionosphere, and electric currents. And it continues contributing to geomagnetism and ionospheric science fields.
Each of the three satellites of the Swarm constellations carries onboard a set of instruments to achieve the mission objectives: a Vector Field and an Absolute Scalar Magnetometer (VFM and ASM); three star trackers (STR) for accurate attitude determination and, recently, for energetic particle detection; a dual-frequency GPS receiver (GPSR); an accelerometer (ACC); an Electric Field Instrument (EFI), composed of two Langmuir Probes (LPs) and two Thermal Ion Imagers (TIIs), dedicated to electric field and plasma measurements. The products derived from EFI instruments represent the focus of this work.
A defining feature of the Swarm mission is its commitment to continuous improvement. Since its launch, advancements in data processing algorithms have been continuously applied: these updates have not only maintained the good quality of Swarm's measurements but have also allowed the mission to evolve and continue meeting the needs of the scientific community. These refinements served the development of novel Swarm-based data products and services, further broadening the mission’s impact, and allowing it to overcome the initial objectives and go beyond its original scope, such as in the Space Weather field.
In December 2025, the most recent baseline has been transferred to operations, delivering updated datasets and evolved products. These algorithm updates greatly impacted the EFI LP products. This work will provide an overview of the improvements applied on Swarm plasma data products: detailed analyses are presented, dedicated to new plasma densities and temperatures parameters, new flags, and other upgrades; comparisons with other L1B and L2 Swarm products are performed; case studies in correspondence of recent main Space Weather events are also displayed, to highlight the innovative application of Swarm to this field.
How to cite: Forte, R., Qamili, E., Panebianco, V., Mizerska, A., Partous, F., Buchert, S., Förster, M., Trenchi, L., Maltese, A., Tøffner-Clausen, L., Olsen, N., Stromme, A., and De la Fuente, A.: Swarm Electric Field Instruments, processors and data quality: evolutions, new baseline and scientific highlights, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-11552, https://doi.org/10.5194/egusphere-egu26-11552, 2026.
The VirES service launched publicly in 2016 and has continuously evolved, adding more datasets and features every year [1]. It comprises four main components: server, web client, Python client, and JupyterHub, providing a range of routes to access, visualise, and process the Swarm product portfolio [2] and more.
Notable features include:
- LEO magnetometry from other missions: CHAMP, CryoSat-2, GRACE, GRACE-FO, GOCE
- INTERMAGNET ground observatories
- Notebook-based cookbook [3]
- Heliophysics API (HAPI) [4]
Building upon robust data access via VirES and HAPI, Swarm DISC (Swarm Data, Innovation, and Science Cluster) is also developing the SwarmPAL Python package [5] to facilitate higher-level analysis. Overall, we aim to produce a sustainable ecosystem of tools and services, which together support accessibility, interoperability, open science, and cloud-based processing [6]. All services are available freely to all, and the software is developed openly on GitHub [7,8].
The work presented is the result of many partners across Swarm DISC.
[1] https://vires.services/changelog
[2] https://swarmhandbook.earth.esa.int
[3] https://notebooks.vires.services
[4] https://vires.services/hapi
[5] https://swarmpal.readthedocs.io
[6] https://doi.org/10.3389/fspas.2022.1002697
[7] https://github.com/ESA-VirES
[8] https://github.com/Swarm-DISC
How to cite: Pačes, M. and Smith, A.: ESA's VirES for Swarm service in 2026, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-13435, https://doi.org/10.5194/egusphere-egu26-13435, 2026.
Swarm Investigation of SpAce Weather and NAtural HazaRds Effects (Swarm-AWARE) is a new European Space Agency (ESA) project funded by the Earth Observation (EO) Science for Society programme. The main goal of the Swarm-AWARE project is to apply innovative techniques and deliver new scientific discoveries of the Earth system, pertinent to space weather (SWE) and natural hazards (NH) effects. Relevant achievements are expected through a systematic investigation of Swarm-derived indices related to magnetospheric substorm activity, field-aligned currents (FACs), magnetic storm activity, ultra-low frequency (ULF) plasma waves and equatorial Spread-F (ESF) events (plasma bubbles). Both the SWE and NH scientific targets have great societal impacts, since SWE effects can include damage and disruption to power distribution networks on the ground, while NH can result in a broad range of effects, from various perturbations of the ionosphere and related disruptions of, e.g., positioning (GPS, GNSS, Galileo) or telecommunication services (notably affected also by strong SWE events), up to most severe consequences, including the loss of human lives.
We tackle this great challenge through the use of state-of-the-art machine learning (ML) and advanced time series analysis (TSA) techniques. The Swarm-AWARE project exploits the unique capabilities of the Swarm mission data, including multi-point observations, together, significantly, with complementary ground data (e.g., SuperMAG magnetometer network and all-sky cameras). Furthermore, in addition to exploiting the unique nature of these combined data sets, Swarm-AWARE highlights potential new foci for future Swarm scientific studies. This research also investigates concepts for potentially new Swarm data products, which address the challenges associated with the impact of geological hazards (e.g., earthquakes, volcanic eruptions) at middle to low latitudes. In parallel, by providing longer time series of the Swarm-derived SFAC index, together with Swarm AE-like and Swarm SYM-H-like geomagnetic activity indices, that currently exist, Swarm-AWARE helps to shed new light on the North-South ionospheric asymmetry, in particular at high latitudes.
How to cite: Balasis, G., Slominska, E., Marghitu, O., Papadimitriou, C., Boutsi, A. Z., Blagau, A., Giannakis, O., and Iorfida, E.: Swarm Investigation of Space Weather and Natural Hazards Effects, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-11971, https://doi.org/10.5194/egusphere-egu26-11971, 2026.
The CHAOS-8 geomagnetic field model series describes the time-dependent near-Earth geomagnetic field under quiet conditions since 1999. It is derived from magnetic field observations from low-Earth orbit satellites, such as Swarm, CHAMP, MSS-1, and CSES, as well as annual differences of revised monthly means of ground observatory measurements. Starting with the 8th generation, the series co-estimates a climatological model of the ionospheric E-layer currents with a focus on accounting for their magnetic signals in the polar regions, which can be significant even under quiet and dark conditions. This model follows the AMPS approach (Laundal et al., 2018), utilizing magnetic apex coordinates and magnetic local time to describe large-scale patterns efficiently. Additionally, it uses multiple external parameters, including the Interplanetary Magnetic Field, dipole tilt angle, and magnetosphere-ionosphere coupling functions, to represent variability on seasonal, daily, and shorter time scales.
Although the CHAOS ionospheric field model can successfully represent the average patterns in the polar ionospheric E-layer field, limitations remain. Most notably, it is less suitable at non-polar latitudes, where the Sq current system dominates, because it lacks longitude dependence. Moreover, the reliance on simple dependencies on external parameters to capture temporal variability may be overly restrictive, particularly for seasonal and long-term changes. Finally, since the CHAOS ionospheric field is estimated only from satellite data, both the internal and ionospheric contributions are treated as internal sources.
This work presents ongoing efforts to address limitations in the CHAOS ionospheric field. Test models are estimated from satellite data using monthly and shorter time windows to capture seasonal variability better. Longitudinal dependence is introduced to provide a more accurate representation of the field at low latitudes, following the approach of the comprehensive model (Sabaka et al. 2003), while continuing to rely on apex coordinate systems. By comparing model predictions to ground observatory data, the potential of incorporating observatory measurements into the model estimation is explored to enhance the separation of internal and ionospheric contributions.
How to cite: Kloss, C. and Schejbel Nielsen, N.: New developments of the CHAOS ionospheric field model, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-18081, https://doi.org/10.5194/egusphere-egu26-18081, 2026.
Langmuir probes are instruments devoted to the in-situ measurement of plasma parameters,
such as floating and plasma potentials, as well as density and electrons temperature. Un
derstanding the interactions among this type of payload, the satellite body, and the orbital
environment is crucial to determine whether specific geometries and conditions could create
phenomena that may affect the plasma measurement. A realistic CAD model of an ionospheric
plasma probe is implemented with the SPIS (Spacecraft Plasma Interaction Software) program
ming environment. SPIS, developed by the SPINE community, is used to simulate the mutual
interaction between the satellite and the probe with the ionospheric plasma (LEO) using the
particle-in-cell method. The results of the numerical simulation are then compared with real
satellite data (from Swarm, CSES, and DEMETER missions) and data collected from a similar
instrument of the INAF-IAPS diagnostic system of the INAF-IAPS Plasma Chamber in Rome
How to cite: La Rovere, G., Diego, P., and Piersanti, M.: Identification of the principal characteristics of an ionospheric Langmuir Probe for furture satellite space mission, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-18301, https://doi.org/10.5194/egusphere-egu26-18301, 2026.
Solid-state detectors (SSDs) are commonly used in space environments to detect particles and radiation. The Multiple Particle Analyzer (MPA) is a scientific payload built upon an SSD application. The MPA will be carried on the Formosat-8C satellite (FS-8C) in the future to monitor global ionospheric space weather. Its design was originally derived from the STE (Supra Thermal Electron) detector on the STEREO satellite. This analyzer utilizes a multi-channel detector component that can measure electrons, ions, and neutral atoms in the energy range of approximately 1 to 200 keV. The team from National Cheng Kung University (NCKU) is currently developing and testing the scientific payload, with a flight model of the MPA expected to be submitted in the fourth quarter of 2026. The FS-8C satellite is scheduled to launch at the end of 2027.
How to cite: Chiang, C.-Y., Chang, T.-F., Cheng, Y.-R., Yen, T.-E., Tsai, S.-C., Chen, C.-T., Liu, P.-J., and Cheng, Y.-T.: Development of a Solid-State Detector for Use in Ionospheric Environments, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-19482, https://doi.org/10.5194/egusphere-egu26-19482, 2026.
A recent update of the MCM series of magnetic field models and associated core surface flows is presented. The models were derived sequentially from year 1999 to 2025, using magnetic satellite and ground observatory data. A linear Kalman filter approach and prior statistics based on numerical dynamo runs were used. The core field, the secular variation and the core surface flow models present the same characteristics as previous versions up to 2023 and we investigate how this behaviour evolves over the most recent years. In particular, before 2023 filtering out the flow variation periods longer than ∼11.5 years revealed filtered azimuthal flow with ∼7 years periodicities and patterns propagating westward by ∼60deg longitude per year. Preliminary results show that the same patterns are maintain over the most recent epochs.
How to cite: Lesur, V.: Core magnetic field and associated surface flow variations from 1999 to 2025, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-22028, https://doi.org/10.5194/egusphere-egu26-22028, 2026.
Recent thermospheric wind observation by a balloon borne instrument HIWIND over New Zealand in April 2025 combined with ground based Fabry Perot interferometer observations in Brazil provides a good opportunity to examine the longitudinal variations in the southern mid latitude region. The results showed noticeable longitudinal variations, which could be generated by nonmigrating tides propagating from the lower atmosphere. HIWIND also provided the first southern hemisphere daytime thermospheric wind observations. Combined HIWIND data with COSMIC 2 radio occultation observations of ionosphere profiles in the southern hemisphere we will examine the interaction between the ionosphere and thermosphere. Using the first principle model TIEGCM we simulated the southern hemisphere thermospheric winds and ionosphere profiles to compare with the HIWIND and COSMIC observations. HIWIND results help to reveal significant discrepancy between observations and simulations and point toward the direction for future improvement of the simulations.
How to cite: Wu, Q., Wu, H., and Wang, W.: Thermospheric Wind Longitudinal Variations in the Southern Mid Latitudes, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-2624, https://doi.org/10.5194/egusphere-egu26-2624, 2026.
Magnetosphere and ionosphere coupling is largely driven by electromagnetic waves (e.g., Alfven waves) and particle precipitation in the polar cusp and auroral region. Magnetic perturbations (dB) in the ionosphere span scales from >1,000 km across the auroral zone—associated with Region-1 and Region-2 field-aligned currents (FACs)—down to <1 km, approaching the electron inertial length, corresponding to fine-scale auroral arcs (~100 m). These smaller scale dB are often linked to inertial Alfven waves that carry parallel electric fields, accelerate electrons, and produce dynamic auroral structures. During geomagnetic storms, transient currents associated with these small-scale dB can exceed several hundred μA/m2, leading to significant ionosphere total electron content (TEC) perturbations and plasma irregularities that cause GPS scintillations and disrupt communication. However, it remains a challenge to fully understand how these small-scale FACs and associated particle precipitation drive ionosphere irregularities and GPS scintillations. NASA's TRACERS mission, launched on 23 July 2025, offers new opportunities to address this problem. We present initial observations from TRACERS showing coincident small-scale dB, particle precipitation, and strong GPS scintillation events in the nightside auroral and dayside cusp regions.
How to cite: Shen, Y., Strangeway, R., Cao, H., Weygand, J., Wu, J., Halekas, J., Fuselier, S., McCaffrey, A., Jayachandran, P., Billett, D., Watson, C., Miles, D., Bonnell, J., Roglans, R., and Hospodarsky, G.: Ionosphere small-scale magnetic perturbations associated with GPS scintillations in the auroral and cusp regions, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-4332, https://doi.org/10.5194/egusphere-egu26-4332, 2026.
Accurate forecasting of Thermospheric Neutral Density (TND) is essential for Low-Earth Orbit (LEO) mission planning, collision avoidance, and orbit determination. Atmospheric drag strongly influences satellite trajectories below 1000 km altitude, making precise density estimates critical for operational safety. Current empirical and physics-based modelsoften show limited skills to capture short-term variability driven by solar and geomagnetic activity. This limitation reduces their accuracy during dynamic space weather conditions and impacts mission planning.
We propose an adaptive machine learning framework using Extreme Gradient Boosting (XGBoost) to predict the systematic deviations from NRLMSISE-2.1 in log space. The model combines GRACE accelerometer-derived TND observations for the years 2009-2017, CODE's global TEC maps, and space weather indices represented by indices such as F10.7 and Ap. Feature engineering incorporates diurnal and seasonal cycles, altitude dependence, and ionosphere-thermosphere coupling. We apply lagged TEC and geomagnetic indices for short-term memory without needing sequential models. This ensures that this approach stays compatible with tabular workflows and keeps them computationally efficient.
A warm-start learning scheme is introduced tofacilitate short-term adaptation through fine-tuning the model with respect to the most recent observations. Validation on the GRACE and Swarm datasets shows an improvement compared to the original NRLMSISE-2.1 model. The reduction in RMSE is approximately 60-70%, and a MAPE improvement of a similar margin is seen under quiet conditions. Storm-time robustness has also been improved. The model performs well when validated on an off-track manner to validate its spatial generalization properties beyond the nominal orbit covered by the GRACE mission. The RMSE reduction is approximately 40%,
These results highlight the potential of AI-driven approaches for operational thermospheric density forecasting. Improved accuracy supports orbit prediction, drag estimation, and space weather applications. The novel framework combines robustness, adaptability, and computational efficiency. This makes it appropriate for integration into real-time mission planning and collision avoidance systems.
How to cite: Thomsen, L. A. and Foorotan, E.: Adaptive AI Forecasting of Thermospheric Neutral Density Tuned to GRACE Data, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-4384, https://doi.org/10.5194/egusphere-egu26-4384, 2026.
Launched by the European Space Agency (ESA) in November 2013, the three-satellite Swarm constellation continues to deliver high-quality measurements of Earth’s magnetic field and the surrounding plasma environment. After more than 12 years in orbit, the mission has achieved remarkable scientific results, deepening our understanding of geomagnetic field dynamics and supporting applications that go well beyond the mission’s original goals.
Equipped with 7 complementary instruments each spacecraft — including a Vector Field and an Absolute Scalar Magnetometer (VFM and ASM); star trackers (STR); a dual-frequency GPS receiver (GPSR); an accelerometer (ACC); an Electric Field Instrument (EFI), composed of two Langmuir Probes (LPs) and two Thermal Ion Imagers (TIIs) — Swarm has become a pivotal reference for geophysical research, supporting advances in areas such as core dynamics, ionospheric and magnetospheric processes, space weather monitoring, and the characterization of electric currents throughout the Geospace environment.
This paper presents a comprehensive overview of the current status of the Swarm mission and constellation, with particular focus on the long-term performance, stability, and calibration of its instruments. The discussion highlights how the constellation’s unique configuration and consistently high data quality have ensured the continuity and reliability of key geophysical observations for more than a decade, with a look at plans for the next future of the mission.
Furthermore, we outline the significant enhancements introduced with the latest Swarm data-processing baseline, which improves the accuracy, consistency, and overall usability of the mission’s data products.
How to cite: Qamili, E., Strømme, A., Olsen, N., Forte, R., Panebianco, V., Tøffner-Clausen, L., Bregnhøj Nielsen, J., Buchert, S., Siemes, C., Mizerska, A., Partous, F., Iorfida, E., Trenchi, L., and de la Fuenete, A.: Swarm After 12 Years in Orbit: Mission Status, Instrument Performance, and Data Quality, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-10534, https://doi.org/10.5194/egusphere-egu26-10534, 2026.
Field-aligned currents (FACs) are a primary channel for the transport of energy and momentum from the magnetosphere into the ionosphere, where they strongly influence atmospheric dynamics through Joule heating. Due to significant spatial and temporal variability, accurately determining FAC density vectors from magnetic field measurements remains challenging. Amongst available techniques, the curlometer method applied to multi-spacecraft magnetic field observations provides the most reliable means of estimating current density. A full three-dimensional reconstruction requires magnetic field measurements at four distinct locations arranged in a near-regular tetrahedral configuration. In contrast, configurations involving fewer spacecraft may be employed, though this approach relies on the assumption of magnetic field stationarity and favourable spacecraft alignment. Here, we investigate current density reconstruction from Swarm magnetic field measurements and evaluate associated quality metrics for a range of conditions for scenarios, spanning macro-, meso-, and micro-scale FAC structures during geomagnetic storms. We then apply this method to simulated trajectories of the tetrahedral configuration proposed for the ROARS F3 mission concept, quantifying the improvements in FAC estimation enabled by a dedicated four-spacecraft mission to Low Earth Orbit.
How to cite: Gajewski, R. and Desai, R.: Multi-scale Reconstruction of Field-Aligned Currents Using the Swarm Spacecraft, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-12104, https://doi.org/10.5194/egusphere-egu26-12104, 2026.
This presentation provides an overview and update on the Canadian Space Agency sponsored IMAGER project, which has two main objectives: 1) Fly an upgraded ionospheric ion analyzer (the 'MPI') on the CalgaryToSpace FrontierSat cubesat to characterize ionospheric flows in the vicinity of the aurora and STEVE and investigate satellite charging; 2) Develop and fly an improved analyzer to measure ionospheric ion drift as part of the Swedish SYSTER suborbital rocket mission to investigate ionosphere-thermosphere coupling. The design, development, integration and test activities are conducted by students in the spirit of the training component of CSA's Flights and Fieldwork for the Advancement of Science and Technology (FAST) programme. FrontierSat and SYSTER are scheduled for launches in 2026. We introduce each mission's scientific rationale, highlight recent technical and training developments, and briefly describe several potential future mission opportunities in upper-atmospheric cold-plasma physics.
How to cite: Burchill, J., Beer, K., Borges, V., Desai, R., Ivchenko, M., Knudsen, D., Rupprecht, C., Sarris, T., and Spanswick, E.: Innovative Measurements of Auroral Geophysics for Education and Research (IMAGER), EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-13271, https://doi.org/10.5194/egusphere-egu26-13271, 2026.
High-latitude field-aligned currents (FACs) reflect, in steady-state, the force balance between magnetospheric plasma dynamics and the collisional coupling of plasma to the neutral atmosphere in the ionosphere. Assessing the impact of high-latitude FACs at low latitudes is difficult for at least two reasons. First, FACs are primarily inferred from magnetometer measurements in low-Earth orbit by estimating the radial current using horizontal magnetic field perturbations and converting it to a FAC using a geometric factor. While this yields a locally correct estimate of the FAC density, the magnetic field generated by a radial current system differs from that generated by the corresponding FAC system when field lines are not radial. As a result, the magnetic field of the horizontal component of FACs, including their remote magnetic field observed at low latitudes, are neglected. Second, in many numerical simulations, FACs are coupled to the ionosphere only at high latitudes, while boundary conditions are imposed at lower latitudes, arguably making it difficult, from a fundamental physics perspective, to trace how high-latitude forcing influences low latitudes.
Here we use AMPERE estimates of high-latitude FACs at 10-min resolution derived from magnetometer measurements on the Iridium satellite constellation to quantify their low-latitude impact. FACs in both polar regions are used to calculate the remote magnetic field using the integration method of Engels and Olsen (1998, https://doi.org/10.1016/S1364-6826(98)00094-7). A recently developed magnetosphere-ionosphere coupling model (Laundal et al. 2025, https://doi.org/10.5194/angeo-43-803-2025) is used to compute the associated penetration electric field. The resulting magnetic and electric fields are compared with observations at low latitudes.
How to cite: Laundal, K. M., Skeidsvoll, A., Braileanu, B., Hatch, S., Olsen, N., Waters, C., Madelaire, M., Kebede, F., Finlay, C., Kloss, C., and Gjerloev, J.: Low-latitude effects of high-latitude field-aligned currents, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-17103, https://doi.org/10.5194/egusphere-egu26-17103, 2026.
Posters virtual: Mon, 4 May, 14:00–18:00 | vPoster spot 1a
EGU26-8566 | Posters virtual | VPS29
Pc3 geomagnetic pulsations excited by earthquakes and their commonality with solar wind-originated Pc3Mon, 04 May, 14:09–14:12 (CEST) vPoster spot 1a
The source of compressional Pc3 magnetic pulsations has been considered to be the plasma process in the solar wind or in the magnetosphere. However, we found some strong inland earthquakes that occur on the dayside also excite Pc3s. The Lamb waves generated by the January 2022 Tongan undersea volcanic eruption are also believed to have excited large amplitude and short period compressional Pc3 geomagnetic pulsations in the dayside plasmasphere (Iyemori et al., 2025). Increases in power spectral density (PSD) in the Pc3 frequency band were observed 10-30 minutes after the origin time of large inland earthquakes (M>6.5) during the daytime (10-14 LT). During these large earthquakes, seismic waves with period of 10-30 seconds propagate far away (even more than several thousand km), causing slight fluctuations in the orientation of magnetometer sensors, resulting in apparent Pc3-like fluctuations. To avoid such sensor tremor effect, we analyzed the total force of magnetic field, or analyzed comparing with seismometer data. We also used the Swarm satellite observation. The PSD of Pc3s caused by earthquakes or by Lamb wave show many spectral peaks having interval of 3-5 mHz, and this is similar with the characteristic reported by, for example, Samson et al. (1995) for normal, i.e., solar wind origin Pc3s. In this paper, we will also show the commonality between the Pc3s caused by earthquakes or Lamb waves and those originated from the solar wind and discuss what the commonality means.
How to cite: Iyemori, T., Aoyama, T., and Yokoyama, Y.: Pc3 geomagnetic pulsations excited by earthquakes and their commonality with solar wind-originated Pc3, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-8566, https://doi.org/10.5194/egusphere-egu26-8566, 2026.
EGU26-18706 | ECS | Posters virtual | VPS29
SwarmDF: A toolbox for analysing high-latitude ionospheric electrodynamicsMon, 04 May, 14:12–14:15 (CEST) vPoster spot 1a
The Swarm Data Fusion (SwarmDF) toolbox is designed as an easy-to-use Python module for analysing the local electrodynamics of the high-latitude ionosphere by combining measurements from ESA’s Swarm satellites with additional ionospheric and thermospheric datasets. Given a Swarm satellite ID, a regional grid, and a time interval, the toolbox automatically retrieves and combines available observations from SuperDARN, SuperMAG, Iridium/AMPERE, and Swarm electromagnetic field measurements. SwarmDF uses the local mapping of polar ionospheric electrodynamics (Lompe) technique to reconstruct two-dimensional maps of key electrodynamic parameters in the vicinity of the Swarm satellite tracks. To assess and quantify reconstruction performance, SwarmDF integrates the LompeOSSE Python module, which generates controlled synthetic electrodynamics datasets based on Gamera simulations and enables systematic comparisons with the toolbox outputs under different data availability and configuration scenarios. Featuring a user-friendly graphical interface, SwarmDF simplifies data handling and model setup for high-latitude ionospheric electrodynamic studies using Swarm observations.
How to cite: Decotte, M., Laundal, K. M., and Kebede, F. T.: SwarmDF: A toolbox for analysing high-latitude ionospheric electrodynamics, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-18706, https://doi.org/10.5194/egusphere-egu26-18706, 2026.
