This session traditionally provides a forum for the discussion of all aspects of solar and heliospheric physics. Popular topics have included solar cycle dependencies of the Sun, solar wind and heliosphere, Coronal Mass Ejection research, studies of energetic particles throughout the heliosphere, and the outer boundaries of the heliosphere. We encourage contributions related to all ongoing and planned space missions, to ground-based experiments and to theoretical research. Papers presenting ideas for future space missions and experiments are very welcome in this session. The session will consist of both oral and poster presentations.

The Sun’s atmosphere is the birthplace of multi-scale magnetic activity (e.g., flares, CMEs, jets, waves, and radio emissions). This activity drives challenging phenomena such as the heating and acceleration of the solar wind, energetic particles, and space weather impacting the whole heliosphere. Parker Solar Probe (PSP) is the first human-made object diving into the solar corona. By the EGU 2023, PSP would have completed 15 of its 24 planned orbits. PSP flew as close as 13.28 solar radii from the Sun’s center as it inches closer to its ultimate perihelion of 9.86 solar radii on 24 December 2024. PSP launched during solar activity minimum and is now experiencing increasing solar activity as the solar cycle climbs to its maximum around 2024-25. PSP data have already led to fundamental new insights into the processes driving the solar wind, CMEs, and SEPs. Remote sensing observations of the solar corona from within the Alfvén critical boundary yielded spectacular fine structures of coronal outflows not visible from 1 au. Beyond breakthroughs in solar and heliospheric physics, PSP has facilitated discoveries in the physics of planets, asteroids, comets, and dust particles. Combining the PSP and SolO observations with observations from other space-born missions and ground-based observatories (e.g., SDO, STEREO, Proba2, ACE, WIND, DSCOVR, and DKIST) and with theoretical models currently in development promise a wealth of further exciting findings. This session invites scientific contributions to all aspects of research addressed to exploring the inner heliosphere and solar corona, with a particular focus on the new observations from PSP and SolO and other complementary observations and models. The session is in collaboration with the special session dedicated to the Solar Orbiter.

Solar Orbiter is an ESA/NASA's Sun orbiting mission that was launched in February 2020. After a successful commissioning phase, the nominal science phase of the mission started in November 2021. The six remote sensing and four in situ instruments onboard Solar Orbiter provide game-changing observations for the study of the connection between the Sun and the heliosphere. During the mission, Solar Orbiter undergoes close approaches to the Sun as well as periods when the orbit comes out of the ecliptic plane. During these periods of high opportunity for new observations and discoveries, observation campaigns coordinating onboard instruments and other space and ground-based assets are performed. The presentations of this session will focus on observations performed during the nominal phase of the mission, and in particular on the first two perihelia, around the 26 March and 13 October 2022, when Solar Orbiter reached 0.32 and 0.29 AU, respectively.

Activities including the recent ESA Voyage 2050 exercise and the ongoing Heliophysics Decadal Survey in the US have triggered various new ideas on fundamental science themes in the area of solar, solar wind, magnetosphere, ionosphere-thermosphere physics at Earth and different planets, plasma physics around the moon and small body, as well as in the heliospheric boundary region. While the idea of implementation scheme (mission) may differ, there are commonality in the underlying physical processes of interest. Discussing the outstanding problems throughout the heliosphere by bringing the different discipline should bring us new perspective of the broad science area. In this session we invite papers which highlight the outstanding science questions in the different area of space plasma physics throughout the solar system and beyond. Ideas on new observations in space and from ground, new modeling, suggestions on new data analysis schemes are also welcome. We welcome active participation of Early Career Scientists and experts from the broad international heliophysics community

Solar Irradiance is the key energy input to Earth. A positive Earth Energy Imbalance (EEI) is the energy, which is continuously stored by the Earth and will ultimately be released to the atmosphere, causing global warming. In order to determine its exact value both the Total Solar Irradiance (TSI) and the Top of the Atmosphere (ToA) Outgoing Radiation (TOR) need to be measured with unprecedented accuracy and precision. This calls for improved instrument technologies as well as a traceable calibration chain of the space instrumentation. In this session we invite contributions on both the measurement and modeling of total and spectral solar irradiance and their effects on the Earth's atmosphere and climate, as well as latest measurements and modelling efforts to determine the Earth's outgoing radiation and the energy storage in the Earth's system.

The solar wind is a continuous plasma flow that fills the heliosphere and is crossed by strong transient perturbations such as interplanetary shocks, coronal mass ejections (CMEs), and (corotating) stream interaction regions (SIRs). These phenomena are capable of driving large disturbances at Earth as well as at the other planets. Understanding their physical behaviour and making accurate predictions about their properties and evolution is a difficult and ongoing issue in heliophysics. Remote-sensing and in-situ measurements from multiple vantage points, combined with ground-based observations and modelling efforts, are employed to study the solar wind plasma and CMEs from their onset to their arrival at planets and spacecraft throughout the heliosphere.

Recently launched spacecraft (including Parker Solar Probe, Solar Orbiter, and BepiColombo), “older” existing probes (such as STEREO and the assets near Earth and Mars), as well as planned and future missions present an ideal opportunity to test, validate and refine current knowledge in this field. We therefore encourage submissions with the aim of exploiting the latest observational and modelling efforts regarding CME and solar wind evolution during their propagation throughout the heliosphere. Contributions on novel methodologies and/or mission concepts that may help shed light on withstanding questions on the matter are also welcome.

The "Theory and Simulation of Solar System Plasmas" session solicits presentations of the latest results from theoretical investigations and numerical simulations in space plasma-physics from microscopic to global scales, in comparison with experiments and observations in the heliosphere: at the Sun, in the solar corona, in interplanetary space and in planetary magnetospheres. This provides a forum to present advances in plasma theory relevant to current and future space missions, such as MMS, Parker Solar Probe, Solar Orbiter and ASO-S, as well as space exploration including space stations, the moon and Mars. Each year a topic of special interest is chosen as a focus of the session. For 2023, this focus will be on the sun and solar wind. Of particular interest is to understand magnetic reconnection, plasma heating and particle acceleration processes as well as the resulting observable radiation processes.

The heliosphere is permeated with energetic particles of different compositions, energy spectra and origins. Two major populations of these particles are galactic cosmic rays (GCRs), which originate from outside of the heliosphere and are constantly detected at Earth, and solar energetic particles (SEPs) which are accelerated at/near the Sun during solar flares or by shock fronts associated with the transit of coronal mass ejections. Enhancements in energetic particle fluxes at Earth pose a hazard to humans and technology in space and at high altitudes. Within the magnetosphere, energetic particles are present in the radiation belts, and particle precipitation is responsible for the aurora and for hazards to satellites. Energetic particles have also been shown to cause changes is the chemistry of the middle and upper atmosphere, thermodynamic effects in the upper troposphere and lower stratosphere region, and can influence components of the global electric circuit. This session will aim to address the transport of energetic particles through the heliosphere, their detection at Earth and the effects they have on the terrestrial atmosphere when they arrive. It will bring together scientists from several fields of research in what is now very much an interdisciplinary area. The session will allow sharing of expertise amongst international researchers as well as showcase the recent advances being made in this field, which demonstrate the importance of the study of these energetic particle populations.

Space and astrophysical plasmas are typically in a turbulent state, exhibiting strong fluctuations of various quantities over a broad range of scales. These fluctuations are non-linearly coupled and this coupling may lead to a transfer of energy (and other quantities such as cross helicity, magnetic helicity) from large to small scales and to dissipation. Turbulent processes are relevant for the heating of the solar wind and the corona, acceleration of energetic particles. Many aspects of the turbulence are not well understood, in particular, the injection and onset of the cascade, the cascade itself, the dissipation mechanisms, as well as the role of specific phenomena such as the magnetic reconnections, shock waves, expansion, and plasma instabilities and their relationship with the turbulent cascade and dissipation.
This session will address these questions through discussion of observational, theoretical, numerical, and laboratory work to understand these processes. This session is relevant to many currently operating missions (e.g., Wind, Cluster, MMS, STEREO, THEMIS, Van Allen Probes, DSCOVR) and in particular for the Solar Orbiter and the Parker Solar Probe.

Space, laboratory, and astrophysical plasmas are seemingly different environments, which however host very similar processes: among them, turbulence, magnetic reconnection, kinetic instabilities and shocks, which all result in particle acceleration and plasma heating. These processes are highly non-linear, and closely interlinked. On one hand, the turbulence cascade favors the onset of magnetic reconnection between magnetic islands and, on the other hand, magnetic reconnection can trigger turbulence in the reconnection outflows and separatrices. Similarly, shocks may form in collisional and collisionless reconnection processes and can be responsible for turbulence generation, as for instance in the turbulent magnetosheath.
The investigation of these processes based on simulations and observations are converging. Simulations can deliver output that is approaching, in temporal and spatial scales and in the coexistence of several scales, the complexity of an increasing number of the processes of interest. On the observation side, high cadence measurements of particles and fields, high resolution 3D measurements of particle distribution functions and multipoint measurements make it easier to reconstruct the 3D space surrounding the spacecraft. The ever growing amount of data that both simulations and observations produce can be then combined through and exploited with Artificial Intelligence and Machine Learning methods.
This session welcomes numerical, observational, and theoretical works relevant for the study of the above mentioned plasma processes. Particularly welcome this year will be works focusing on the common aspects of turbulence, reconnection, and shocks in space, laboratory, and astrophysical plasmas.

This open session traditionally invites presentations on all aspects of the Earth’s magnetospheric physics, including the magnetosphere and its boundary layers, magnetosheath, bow shock and foreshock as well as solar wind-magnetosphere-ionosphere coupling. We welcome contributions on various aspects of magnetospheric observations, remote sensing of the magnetosphere’s processes, modelling and theoretical research. The presentations related to the current and planned space missions and to the value-added data services are also encouraged. This session is suitable for any contribution which does not fit more naturally into one of the specialised sessions and for contributions of wide community interest.

Upstream from the bow shock, some incident solar wind particles can be reflected and under specific geometrical conditions, travel upstream along the magnetic field lines, interact with the solar wind and cause a variety of instabilities and waves before getting carried back to the shock. This complex interaction gives rise to the foreshock environment, where several phenomena take place. These include whistler and ULF waves, hot flow anomalies (HFAs), spontaneous hot flow anomalies (SHFAs), foreshock cavities, foreshock bubbles, shocklets, and short-large amplitude magnetic structures (SLAMS).

Such foreshock structures appear to govern much of the dynamics upstream of the planetary bow shocks, while modulating the downstream magnetosheath region. They may cause high-speed plasma jets and plasmoids downstream of the shock, or even get directly transmitted through the bow shock. Understanding the coupling between these processes and revealing their effects with respect to the magnetosphere is crucial for the accurate determination of a planetary geospace environment and for quantifying possible space weather effects. On a more fundamental level, such structures and their relation can be connected to phenomena such as magnetic reconnection, particle acceleration and the magnetosphere-ionosphere coupling.

Contributions to this session can include theoretical works, computer simulations, numerical modeling, machine learning applications and observational research. We particularly encourage presentations using data from Terrestrial missions of MMS, THEMIS, and Cluster missions in conjunction with other missions such as Arase (ERG), Van Allen Probes (VAPs) and ground magnetometers. Of particular interest are works that study transient phenomena close to the bow shock of other planetary environments such as Mercury, Venus, and Mars using simulations or observational measurements.

Large-scale dynamic processes in different magnetospheric regions, e.g., at the magnetopause, in the dayside magnetosphere, magnetotail, ring current, plasmasphere, and ionosphere, are closely interconnected therefore the magnetosphere should be considered as a global system. The state of the magnetosphere is controlled mainly by solar wind conditions. The interplanetary magnetic field (IMF) and solar wind plasma parameters control the energy input into the magnetosphere. Magnetic reconnection at the dayside magnetopause and in the tail current layer regulates energy transfer through the magnetosphere. Changes in the solar wind dynamic pressure and IMF move the magnetopause, causing global magnetospheric expansions and contractions. Variations in the solar wind velocity and IMF direction may also displace the magnetotail. Magnetic reconnection in the magnetotail injects thermal and energetic particles into the inner magnetosphere and downward along magnetic field lines into the ionosphere. On the other hand, the polar wind from the upper atmosphere may influence the nightside reconnection rate. Global magnetospheric dynamics can be studied by means of numerical simulations (MHD or kinetic), using empirical and semi-empirical models, or with the help of multipoint in situ spacecraft observations. Arrays of ground-based observatories and a fleet of various space missions can image magnetospheric and ionospheric phenomena globally, providing crucial information concerning the positions and dynamics of the magnetospheric plasma boundaries and the global distribution of ionospheric currents, convective flows, and particle precipitation. Past and future global imaging missions (e.g., TWINS, LEXI, SMILE) can complete this picture providing large-scale snapshots of some geospace regions. Accurate modelling of global magnetospheric processes is an essential condition for successful space weather predictions. We welcome any work presenting results on the global dynamics of the Earth’s magnetosphere as well as the magnetospheres of other planets.

The Earth's inner magnetosphere contains different charged particle populations, such as the Van Allen radiation belts, ring current particles, and plasmaspheric particles. Their energy range varies from eV to several MeV, and the interplay among the charged particles provides feedback mechanisms that couple all those populations together. Ring current particles can generate various waves, for example, EMIC waves and chorus waves, which play important roles in the dynamic evolution of the radiation belts through wave-particle interactions. Ring current electrons can be accelerated to relativistic radiation belt electrons. The plasmaspheric medium can also affect these processes. In addition, precipitation of ring current and radiation belt particles will influence the ionosphere, while up-flows of ionospheric particles can affect dynamics in the inner magnetosphere. Understanding these coupling processes is crucial.

While the dynamics of outer planets’ magnetospheres are driven by a unique combination of internal coupling processes, these systems have several fascinating similarities which make comparative studies particularly interesting. We invite a broad range of theoretical, modeling, and observational studies focusing on the dynamics of the inner magnetosphere of the Earth and outer planets, including the coupling of the inner magnetosphere and ionosphere and coupling between the solar wind disturbances and various magnetospheric processes. Contributions from all relevant fields, including theoretical studies, numerical modeling, and observations from satellite and ground-based missions are welcome. In particular, we encourage presentations using data from MMS, THEMIS, Van Allen Probes, Arase (ERG), Cluster, cube-sat missions, Juno, SuperDARN, magnetometer, optical imagers, IS-radars, and ground-based VLF measurements.

The Earth's ionosphere embedded in the thermosphere is a coupled system influenced by Solar activity and magnetospheric processes from above, as well as by upward propagating disturbances from lower atmospheric layers. This open session is suitable for contributions on all aspects of ionospheric and thermospheric physics, in particular concerning ionospheric disturbances of different origin and their effects on modern human technologies. The session invites theoretical studies, (multi)instrumental ground-based and space-based observations, simulations and modelling studies that address the dynamics of the ionosphere, concerning transient events, plasma waves and irregularities, as well as large-scale dynamics and ionospheric and thermospheric climate. Contributions dealing with magnetospheric forcing are sought in the areas of ionospheric disturbances caused by CME- and CIR/CH HSS-related storms and substorms. New results that focus on investigation of latitudinal, seasonal and hemispheric differences in ionospheric response to storm induced disturbances are especially appreciated. Also ionospheric effects from other sources, such as the solar terminator, solar eclipses, seismic activity or antropogetic explosions, are welcome. As for forcing by the lower atmosphere, contributions are sought that focus on atmospheric waves, wave-wave and wave-mean flow interactions, atmospheric electricity and electrodynamic coupling processes.

The ionosphere is a highly complex plasma containing electron density structures spanning a wide range of spatial and temporal scales. Large scale structures with horizontal extents of tens to hundreds of km exhibit variation with time of day, season, solar cycle, geomagnetic activity, solar wind conditions and location. Smaller scale structures can be seeded from these larger scale structures or can be driven directly. Collectively, these structures can be driven from above, enabling discoveries about the coupling of the near-space environment to the Earth’s atmosphere. They can also be driven from below, enabling discoveries about vertical coupling within the atmosphere. The ionosphere is heavily influenced by neutral atmosphere in which it is embedded. The thermosphere can influence the ionosphere, and observations of the ionosphere can be used to infer properties of the thermosphere. We invite studies of the ionosphere and its drivers at any temporal or spatial scale. Contributions which span or compare multiple scale sizes are particularly welcome.

The ionosphere-thermosphere system is the portion of geospace where the neutral atmosphere interacts with plasma. These interactions are driven by numerous periodic and transient processes across broad temporal and spatial scales. Our session aims to communicate the recent advances in atmosphere-ionosphere couplings. We solicit observational and modeling studies on relevant couplings through, e.g., long-term trends, regular atmospheric circulation and oscillations (e.g., the El Niño–southern oscillation and the quasi-biennial oscillation), geological and meteorological transient atmospheric disturbances (e.g., sudden stratospheric warmings, volcanic eruptions, and earthquakes), waves and wave-like perturbations (e.g., planetary waves, tides, gravity waves, and traveling ionospheric disturbances), and turbulent and other nonlinear processes.

The Earth's mesosphere and lower thermosphere (MLT) region is a great platform to study ionospheric dynamics, disturbances, eddy mixing, and controlling parameters. This transition region is sandwiched between the lower and upper atmosphere, which is strongly driven by the forcing from both the above (e.g., solar and magnetospheric inputs) and below (e.g., gravity waves and atmospheric tides). The thermal structure of the MLT region is controlled by numerous sources and sinks of energy, including solar radiation, chemical, and dynamical processes. Solar atmospheric tides related to global-scale variations of winds and waves are responsible for coupling the lower and upper layers of the atmosphere. During this coupling process, the precipitation of energetic particles into the MLT region also greatly influences the vertical profiles of the temperature, chemistry, and dynamics of the upper atmosphere. This is an appropriate forum/time to encourage the scientific community to present, discuss, update, and improve our understanding of dynamics, chemistry, and coupling in the MLT region which ultimately affect the electrodynamics of the whole coupled geospace environment. This session invites presentations on scientific work related to various experimental/observational techniques, numerical and empirical modeling, and theoretical analyses on the dynamics, chemistry, and coupling processes in the altitude range of ~ 60 km – 180 km of the MLT regions.

The Earth’s upper atmosphere and ionosphere are subject to significant variability associated with solar forcing. While in situ observations of the ionosphere-upper atmosphere are only possible with spacecraft and sounding rockets, a wealth of information is obtained thanks to remote sensing techniques using ground-based instruments.
For instance, ground-based magnetometers, used in dense networks, routinely enable the derivation of ionospheric currents and geomagnetic indices. Optical instruments not only provide measurements of auroral and airglow emissions, but are also used to observe upper atmospheric winds and temperatures, e.g. in the thermosphere and mesosphere. Such parameters can also be measured with radars, spanning a wide range of active (ionosondes, meteor radars, coherent and incoherent scatter radars, VLF transmitters, Lidars) and passive (riometers, VLF receivers) systems.
Combining ground-based observations from various instruments enables the development of novel data analysis methodologies which in turn enhance our understanding of the underlying physics of space weather and ionosphere-upper atmosphere processes. This includes the study of densities, temperatures and composition of the ionosphere–upper atmosphere, monitoring of its dynamics and chemistry, and measuring of fluxes from precipitating particles and current systems.
In this session, we invite contributions featuring the use of ground-based instruments in studies of the ionosphere–upper atmosphere system across all latitudes and of space weather and ionospheric–atmospheric physics processes of various time and spatial scales.

Coronal mass ejections (CMEs), interplanetary shocks, corotating interaction regions (CIRs) and solar energetic particles (SEPs) are the main drivers of the heliospheric variability. The corresponding geospace disturbances affect a wide range of technological systems in space and on ground, as well as human health. Therefore, the prediction of their arrival and impact is extremely important for the modern space-exploration and electronics-dependent society. Significant efforts have been made in the past decade to develop and improve the prediction capabilities, through both state-of-the art observations and modelling. Although significant progress has been made, many new challenges have been revealed. We are limited in obtaining reliable observation-based input for the models, tracking solar wind transients throughout the heliosphere and reliably evaluating prediction models. These challenges can be tackled by exploiting and improving our existing capabilities, as well as using the out-of-the-box thinking and break from the traditional methods. This session is devoted to provide the overview of the current state of the space weather prediction of the arrival time and impact of various solar wind transients and to introduce new and promising observational and modelling capabilities. We solicit abstracts on observational and modelling efforts, as well as space weather prediction evaluation. With the overview of our current capabilities and possible future prospects we aim to highlight guidelines to the general direction of the future scientific efforts, as well as space-mission planning.

Space Weather (SW) and Space Climate (SC) are collective terms that describe the Sun-Earth system interactions on timescales varying between minutes and decades and include processes at the Sun, in the heliosphere, magnetosphere, ionosphere, thermosphere and at the lower atmosphere. Prediction of the extreme events (forecast and nowcast) and development of the mitigation strategy are vital as the space assets and critical infrastructures, such as communication and navigation systems, power grids, and aviation, are all extremely sensitive to the external environment. Post-event analysis is crucially important for the development and maintenance of numerical models, which can predict extreme SW events to avoid failure of the critical infrastructures.

This session aims to address both the current state of the art of SW products and new ideas and developments that can enhance the understanding of SW and SC and their impact on critical infrastructure. We invite presentations on various SW and SC-related activities in the Sun-Earth system: forecast and nowcast products and services; satellite observations; model development, validation, and verification; data assimilation; development and production of geomagnetic and ionospheric indices. Talks on SW effects on applications (e.g. on airlines, pipelines and power grids, space flights, auroral tourism, etc.) in the Earth’s environment are also welcomed.

Cosmic rays carry information about space and solar activity, and, once near the Earth, they produce isotopes, influence genetic information, and are extraordinarily sensitive to water. Given the vast spectrum of interactions of cosmic rays with matter in different parts of the Earth and other planets, cosmic-ray research ranges from studies of the solar system to the history of the Earth, and from health and security issues to hydrology, agriculture, and climate change.
Although research on cosmic-ray particles is connected to a variety of disciplines and applications, they all share similar questions and challenges regarding the physics of detection, modeling, and the influence of environmental factors.

The session brings together scientists from all fields of research that are related to monitoring and modeling of cosmogenic radiation. It will allow sharing of expertise amongst international researchers as well as showcase recent advancements in their field. The session aims to stimulate discussions about how individual disciplines can share their knowledge and benefit from each other.

We solicit contributions related but not limited to:
- Health, security, and radiation protection: cosmic-ray dosimetry on Earth and its dependence on environmental and atmospheric factors
- Planetary space science: satellite and ground-based neutron and gamma-ray sensors to detect water and soil constituents
- Neutron and Muon monitors: detection of high-energy cosmic-ray variations and its dependence on local, atmospheric, and magnetospheric factors
- Hydrology and climate change: low-energy neutron sensing to measure water in reservoirs at and near the land surface, such as soils, snow pack, and vegetation
- Cosmogenic nuclides: as tracers of atmospheric circulation and mixing; as a tool in archaeology or glaciology for dating of ice and measuring ablation rates; and as a tool for surface exposure dating and measuring rates of surficial geological processes
- Detector design: technological advancements in the detection of cosmic rays and cosmogenic particles
- Cosmic-ray modeling: advances in modeling of the cosmic-ray propagation through the magnetosphere and atmosphere, and their response to the Earth's surface
- Impact modeling: How can cosmic-ray monitoring support environmental models, weather and climate forecasting, agricultural and irrigation management, and the assessment of natural hazards

The increasing amount of data from an increasing number of spacecraft in our solar system shouts out for new data analysis strategies. There is a need for frameworks that can rapidly and intelligently extract information from these data sets in a manner useful for scientific analysis. The community is starting to respond to this need. Machine learning, with all of its different facets, provides a viable playground for tackling a wide range of research questions in planetary and heliospheric physics.

We encourage submissions dealing with machine learning approaches of all levels in planetary sciences and heliophysics. The aim of this session is to provide an overview of the current efforts to integrate machine learning technologies into data driven space research, to highlight state-of-the art developments and to generate a wider discussion on further possible applications of machine learning.

The session solicits contributions that report on nonthermal solar and planetary radio emissions. Coordinated multi-point observations from ground radio telescopes (e.g., LOFAR, LOIS, LWA1, URAN-2, UTR-2) and spacecraft plasma/wave experiments (e.g., BepiColombo, Solar Orbiter, Parker Solar Probe, UVSQ-Sat, Cassini, Cluster, Demeter, Galileo, Juno, Stereo, Ulysses and Wind) are especially encouraged. Presentations should focus on radiophysics techniques used and developed to investigate the remote magnetic field and the electron density in solar system regions, like the solar corona, the interplanetary medium and the magnetized auroral regions. Interest also extends to laboratory and experimental studies devoted to the comprehension of the generation mechanisms (e.g., cyclotron maser instability) and the acceleration processes (e.g., Alfven waves). Further preparations, evaluations, investigations, analyses of forthcoming space missions or nanosatellites (like Juice, SunRISE, UVSQ-Sat NG, Inspire-Sat 7…) are also welcome.

Swarm is ESA's first constellation mission for Earth Observation and consists of three identical spacecraft launched on 22 November 2013. Each of the three Swarm satellites performs high-precision and high-resolution measurements of the strength, direction and variation of the magnetic field, accompanied by precise navigation, accelerometer, plasma and electric field measurements. Each satellite is equipped with magnetic sensors, measuring a combination of various contributing sources: the Earth’s core field, magnetised rocks in the lithosphere, external contributions from electrical currents in the ionosphere and magnetosphere, currents induced by external fields in the Earth’s interior and a contribution produced by the oceans. This session invites contributions illustrating the achievements of Swarm for investigating all types of Earth and near-Earth processes, as well as contributions describing synergies with other missions and ongoing initiatives towards designing innovative new magnetic field measurements missions.

The ionospheres and (induced) magnetospheres of unmagnetized and weakly magnetized bodies with substantial atmospheres (e.g. Mars, Venus, Titan, Pluto and comets) are subject to disturbances due to solar activity, interplanetary conditions (e.g. solar flares, coronal mass ejections and solar energetic particles), or for moons, parent magnetospheric activity. These objects interact similarly as their magnetized counterparts but with scientifically important differences.
As an integral part of planetary atmospheres, ionospheres are tightly coupled with the neutral atmosphere, exosphere and surrounding plasma environment, possessing rich compositional, density, and temperature structures. The interaction among neutral and charged components affects atmospheric loss, neutral winds, photochemistry, and energy balance within ionospheres.
This session invites abstracts concerning remote and in-situ data analysis, modelling studies, comparative studies, instrumentation and mission concepts for unmagnetized and weakly magnetized solar system bodies.

Time series obtained within the different geoscientific disciplines commonly exhibit a large degree of irregularity, complexity and/or nonstationarity. In such cases, the use of classical (linear) concepts for the statistical analysis and modelling of time series (such as power spectra, autoregressive or other linear models) may be insufficient to obtain reliable and correct process-related information from the available data. Conversely, applying emergent concepts developed in fields like dynamical system theory, stochastic processes or computer science may provide useful tools to foster the knowledge discovery from complex geoscientific systems. Many of the corresponding methods from nonlinear time series analysis have meanwhile matured and reached a stage of broad applicability while still undergoing further methodological refinements, extensions and adaptations.

This session brings together researchers developing time series analysis approaches tailored to nonlinear deterministic and/or stochastic dynamical systems with such applying those concepts across the different geoscientific disciplines and beyond. We are confident that methodological knowledge transfer across the different topical fields present at EGU is of utmost relevance to improving our capability, as a community, to derive the most useful pieces of information from the growing amount of available data on various geoscientific phenomena. Therefore, we cordially invite contributions using different types of approaches, including (but not limited to) multi-scale methods for time series, information theoretic concepts, statistical complexity measures, causal inference, state space methods, stochastic process descriptions, etc., addressing recent methodological developments and/or successful applications to time series from any geoscience discipline and beyond.

Geomagnetically Induced Currents (GICs) can damage grounded infrastructure such as high voltage transformers, oil and gas pipelines and rail networks. Understanding their impact is vital for protecting critical national infrastructure from harm and reducing any economic consequences. GICs are caused by geoelectric fields induced in the resistive subsurface of the Earth during periods of rapid change of the magnetic field, typically in geomagnetic storms; however, an increasing body of evidence shows they occur in nominally quiet times too. We seek contributions from studies that measure (directly or indirectly) or model GICs in grounded infrastructure to assess the potential hazard and vulnerability of the infrastructure and to produce reliable models with which to forecast the potential effects of severe space weather events.