The Solar Orbiter mission, an international cooperation between ESA and NASA, is currently orbiting the Sun near the ecliptic at heliocentric distances ranging from 0.95 to 0.29 au. The fourth close perihelion occurred on 2023 October 7 (0.29 au), and the fifth perihelion is scheduled for 2024 April 4.

The overall goal of Solar Orbiter is to understand how the Sun creates and controls the heliosphere. The valuable data set provided so far by the spacecraft’s comprehensive remote-sensing and in-situ instrument payload allows for coordinated observation campaigns including multi-spacecraft analyses.

This session invites contributions that boost the Solar Orbiter objectives, including observations from Solar Orbiter’s unique vantage point (outside of the Earth-Sun line), combinations with other operational spacecraft, numerical simulations and theory developments that enhance our understanding of the connections between the Sun and the Heliosphere.

The "Theory and Simulation of Solar System Plasmas" session aims at presenting recent results related to theoretical investigations and/or numerical modelling of plasmas processes and dynamics of heliospheric plasmas: the Sun and its corona, the solar wind or planetary magnetospheres. Those plasma processes include magnetic reconnection, turbulence, shock waves, plasma instabilities, plasma heating, particle acceleration, radiation, etc. Results using all kind of plasma models are welcome, including fluid or kinetic models, from global to local modelling, but also multi-scale approaches. Of particular interest are applications relevant for the interpretation of in-situ measurements and remote observations from current and future space missions such as MMS, Parker Solar Probe, Solar Orbiter and ASO-S.
The focus of this year's session is space plasma turbulence: their origin, effects and links with other plasma processes, from large/fluid to small/kinetic scales.

The heliosphere is permeated with energetic particles of different origins. Two major particle populations are galactic cosmic rays (GCRs) and solar energetic particles (SEPs). GCRs originate from outside of the heliosphere and are constantly detected at Earth and in the heliosphere. SEP events are outbursts of energetic particles from the Sun, observed in connection with solar flares and coronal mass ejections (CMEs). Large gradual SEP events are associated with fast and wide CMEs and the primary site of their acceleration is at shock waves driven by the CMEs. These particle populations are key components of space weather.

The present solar cycle is unique in capabilities enabled by missions launched to the inner heliosphere (Solar Orbiter, Parker Solar Probe, BepiColombo) providing, for the first time, excellent possibilities for multi-spacecraft studies of SEP events combined with high-cadence, high-resolution solar observations of the eruptions from multiple points of view, including ground-based radio facilities. In addition, the new missions carry instrumentation that can provide in-situ measurements with much higher quality and resolution than so far possible. This has provided unprecedented opportunities to study collisionless shocks and energetic particles also with single-spacecraft heliospheric observations.

At the highest energies, instruments such as AMS-02 aboard the ISS and ground-based neutron monitors can provide information on GCR transport through the heliosphere. High fluxes of energetic particles of the highest energies can pose a severe radiation risk to crewed spaceflight and a significant threat to satellites. Particle precipitation also causes changes in the chemistry of the middle and upper layers of the Earth's atmosphere, thermodynamic effects in the upper troposphere and lower stratosphere region, and can influence components of the global electric circuit.

Several research projects of the EU Framework Programme have made use of these new capabilities and produced exciting scientific results and data analysis tools for the heliophysics community. We solicit contributions on energetic particles and heliospheric shocks, and their effects at Earth and other planets, that make use of the unique observational capabilities of the 25th solar cycle. A special emphasis will be placed on the recent results and prospects stemming from the European projects targeted on these topics, but other contributions are also welcomed.

This session combines advancements in solar and heliospheric science through radio observations and theoretical understanding of the solar wind and its modeling. Covering various wavelengths, from decameter to millimetre (e.g. Low-Frequency Array (LOFAR), Murchison Widefield Array (MWA), Atacama Large Millimetre/submillimeter Array (ALMA), we invite contributions on topics such as solar eruptions, energy transport, non-thermal electron mechanisms, and the development of new radio instruments for the coronal and heliospheric observations. Additionally, we welcome submissions related to understanding the origins, propagation, and evolution of solar wind in the inner heliosphere. This includes theory, data-driven modelling, and/or multiple ground-based or space observations of solar wind from source to in-situ detection such as studies with Parker Solar Probe, Solar Orbiter and BepiColombo. We welcome contributions from researchers at all career stages, especially early-career scientists and students.

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, and the 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. Moreover, the role of specific phenomena such as the magnetic reconnections, shock waves, solar wind expansion, plasma instabilities and their relationship with the turbulent cascade and dissipation are under debate. 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.

Collisionless shocks are ubiquitous in the universe as they are found in different astrophysical environments, from planets to galaxy clusters. Extensive effort has been put into understanding their rich dynamics and their effects on the surrounding environments, such as the generation of foreshocks, turbulent sheaths and characteristic transient phenomena.
Heliospheric shocks are the only ones that are directly accessible by in-situ measurements. Missions, such as Solar Orbiter, STEREO and Parker Solar Probe have deepened our knowledge of interplanetary shocks and the associated regions, while MMS, Cluster, THEMIS, Cassini, Maven and others have done the same for the planetary bow shocks.
Furthermore, thanks to high-performance computing, global and local simulations have played a vital role in resolving major gaps in our knowledge of collisionless shocks.
Despite these efforts, many questions remain open. In particular, we still do not fully understand the mechanisms associated with certain aspects of particle heating and acceleration, wave generation, wave-particle interaction and energy redistribution at shocks.
Additionally, details about how transient structures, such as hot flow anomalies, foreshock bubbles, cavitons, spontaneous hot flow anomalies, magnetosheath jets etc. are formed and how they interact with and impact the near-Earth environment are also largely still unknown. We thus welcome observational, numerical, and theoretical works focusing on the study of plasma processes at collisionless shocks and surrounding regions.

Coronal mass ejections (CMEs) can be listed amongst the most extreme manifestations of the Sun’s dynamic activity and are prominent drivers of space weather disturbances at Earth as well as other solar system bodies. Over the past few decades, remote-sensing and in-situ measurements as well as analytical and MHD modelling efforts have led to remarkable advances in our understanding of CMEs, but many open questions still stand. These include, for example, the formation and eruption mechanism(s) of CMEs, the factors that dictate their early evolution in the solar corona, their detailed 3D configuration as they propagate through interplanetary space, the processes at play during CME interactions with the structured solar wind and/or other transients, and the presence of pre-eruptive properties that can determine CME geoeffectiveness. As we approach the maximum of Solar Cycle 25, it is important to reassess our current knowledge of solar eruptions and to identify promising avenues to further improve our capabilities to observe, analyse, model, and forecast CMEs.

This session solicits contributions that focus on advancing CME science over a wide range of aspects and approaches. Presentations that we welcome include studies that employ remote-sensing and/or in-situ observations, modelling efforts that focus on CME eruption and/or propagation in the corona and heliosphere, and mission concepts that have the potential to significantly advance CME fundamental research. Particular emphasis will be given to contributions that employ novel theories, measurements, and/or techniques.

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 session convenes researchers investigating various aspects of small celestial bodies and dust in planetary atmospheres and surrounding space. Discussions encompass asteroids, comets, meteoroids, meteors, meteorites, dust (including its behavior, charging, lifting, and settling on planetary surfaces), and more. The session emphasizes the multidisciplinary nature of such studies, incorporating laboratory experiments, numerical simulations, and observations. It provides insights into small bodies' evolutionary and compositional aspects, elucidating their role in shaping space environments. We invite presenters to showcase recent and upcoming space missions, warmly welcome early career scientists, foster collaborative ideas, and encourage the presentation of cross-disciplinary research.

The Heliosphere, a dynamic region of space influenced by the Sun's magnetic and solar wind activity, presents an array of unresolved questions and challenges for researchers. From the innermost planets to the outer reaches of the solar system, numerous persisting problems and processes demand attention from experts of various subdisciplines. This interdisciplinary field encompasses solar physics, solar wind interactions, magnetospheres, ionospheres, thermospheres, and plasma physics, extending from Earth to distant moons, small bodies, and the enigmatic heliospheric boundary region.

While mission implementation schemes may vary, a common thread unites the underlying physical processes of interest. Planetary auroras are a prominent example where the interaction of the solar wind or space weather-related activity with the planetary magnetosphere (if present) and subsequently its atmosphere, leads to auroral emissions. These phenomena arise from complex dynamics involving the planetary atmosphere, magnetosphere, and the surrounding plasma environment. This interplay induces photochemical changes in the atmosphere, deposits heat, and contributes to the atmospheric escape of the planets.

Our proposed session aims to facilitate a comprehensive discussion on the future of Heliophysics research and the persistent common questions spanning the entire Heliosphere. A significant part of the session will delve into the diversity of observed auroras in the Solar System and the underlying physics propelling these phenomena. We invite contributions that spotlight unresolved scientific problems in the field of space plasma physics across our solar system. Authors are encouraged to present ideas for innovative spaceborne and ground-based observations, innovative modeling approaches, and novel data analysis methodologies. Early Career Scientists and established experts from the global Heliophysics and planetary science communities are invited to actively participate in this collaborative exploration of our solar system's dynamic and interconnected Heliophysical environment.

The recent growing number of probes in the heliosphere and future missions in preparation led to the current decade being labelled as "the golden age of heliophysics research". With more viewpoints and data downstreamed to Earth, machine learning (ML) has become a precious tool for planetary and heliospheric research to process the increasing amount of data and help the discovery and modelisation of physical systems. Recent years have also seen the development of novel approaches leveraging complex data representations with highly parameterised machine learning models and combining them with well-defined and understood physical models. These advancements in ML with physical insights or physically informed neural networks inspire new questions about how each field can respectively help develop the other. To better understand this intersection between data-driven learning approaches and physical models in planetary sciences and heliophysics, we seek to bring ML researchers and physical scientists together as part of this session and stimulate the interaction of both fields by presenting state-of-the-art approaches and cross-disciplinary visions of the field.

The "ML for Planetary Sciences and Heliophysics" session aims to provide an inclusive and cutting-edge space for discussions and exchanges at the intersection of machine learning, planetary and heliophysics topics. This space covers (1) the application of machine learning/deep learning to space research, (2) novel datasets and statistical data analysis methods over large data corpora, and (3) new approaches combining learning-based with physics-based to bring an understanding of the new AI-powered science and the resulting advancements in heliophysics research.
Topics of interest include all aspects of ML and heliophysics, including, but not limited to: space weather forecasting, computer vision systems applied to space data, time-series analysis of dynamical systems, new machine learning models and data-assimilation techniques, and physically informed models.

The session combines presentations submitted to two sessions, Open Session on the Magnetosphere and Global magnetospheric dynamics in simulations and observations. The Open Session on the Magnetosphere 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. This session welcomes 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.

The Global magnetospheric dynamics session is dedicated to global large-scale magnetospheric dynamics in simulations and observations. The magnetospheric state is mainly controlled by solar wind conditions. However, solar wind properties change when plasma moves through the bow shock and magnetosheath, therefore the magnetic reconnection rate at the dayside magnetopause depends on parameters in the surrounding magnetosheath and magnetosphere. While global magnetospheric dynamics is understood in terms of the Dungey cycle, several open questions remain, including understanding of different magnetospheric regimes and their drivers, ionospheric feedback, and role of Kelvin-Helmholz instability in the energy transfer from the solar wind into the magnetosphere. Global magnetospheric dynamics can be studied by means of sophisticated numerical simulations, with empirical and semi-empirical models, or using multipoint in situ spacecraft observations. Arrays of ground-based observatories and a fleet of 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. Global imaging missions (e.g., TWINS, LEXI, SMILE, EZIE, GEO-X) can complete this picture providing large-scale snapshots of geospace regions. This session welcomes 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 provide 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 for fundamental understanding and for accurate space weather forecasting.

While the dynamics of outer planets’ magnetospheres are driven by a unique combination of internal coupling processes, these systems have a number of fascinating similarities that 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 as well as new mission concepts. In particular, we encourage presentations using data from MMS, THEMIS, Van Allen Probes, Arase (ERG), Cluster, CubeSat missions, Juno, SuperDARN, ground-based magnetometers and optical imagers, IS-radars and ground-based VLF measurements.

Precipitation of particles into planetary atmospheres is a fundamental heliophysics process, driven by dynamic processes on the sun, in the solar wind, and within planetary magnetospheres. At Earth, precipitation transfers energy from the solar wind and magnetosphere into the ionosphere and upper atmosphere. This dynamic coupling between plasma regimes leads to a variety of impacts on the upper atmosphere; from vibrant auroral displays, to generation of ionospheric current systems, and impacts on satellite infrastructure through increased satellite drag. This session takes a system-science perspective on particle precipitation across wide ranging energies and impacts on the atmosphere. We invite presentations which focus on links between the drivers and their relative importance in generating particle precipitation; the spatiotemporal dynamics of large-scale processes such as solar wind structure of geomagnetic storm phase; and the impacts of particle precipitation on atmospheric conductivity, chemistry, and dynamics.

Time series are a very common type of data sets generated by observational and modeling efforts across all fields of Earth, environmental and space sciences. The characteristics of such time series may however vastly differ from one another between different applications – short vs. long, linear vs. nonlinear, univariate vs. multivariate, single- vs. multi-scale, etc., equally calling for specifically tailored methodologies as well as generalist approaches. Similarly, also the specific task of time series analysis may span a vast body of problems, including
- dimensionality/complexity reduction and identification of statistically and/or dynamically meaningful modes of (co-)variability,
- statistical and/or dynamical modeling of time series using stochastic or deterministic time series models or empirical components derived from the data,
- characterization of variability patterns in time and/or frequency domain,
- quantification various aspects of time series complexity and predictability,
- identification and quantification of different flavors of statistical interdependencies within and between time series, and
- discrimination between mere correlation and true causality among two or more time series.
According to this broad range of potential analysis goals, there exists a continuously expanding plethora of time series analysis concepts, many of which are only known to domain experts and have hardly found applications beyond narrow fields despite being potentially relevant for others, too.

Given the broad relevance and rather heterogeneous application of time series analysis methods across disciplines, this session shall serve as a knowledge incubator fostering cross-disciplinary knowledge transfer and corresponding cross-fertilization among the different disciplines gathering at the EGU General Assembly. We equally solicit contributions on methodological developments and theoretical studies of different methodologies as well as applications and case studies highlighting the potentials as well as limitations of different techniques across all fields of Earth, environmental and space sciences and beyond.

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.

The Earth's middle atmosphere, mesosphere, and lower thermosphere (MLT) region provide a great platform for studying ionospheric dynamics, disturbances, eddy mixing, atmospheric drag effects, and space debris tracking. The thermal structure of these regions is influenced by numerous energy sources such as solar radiation, chemical, and dynamical processes, as well as forces from both above (e.g. solar and magnetospheric inputs) and below (e.g. gravity waves and atmospheric tides). Solar atmospheric tides, related to global-scale variations of temperature, density, pressure, and wind waves, are responsible for coupling the lower and upper layers of the atmosphere and significantly impact their vertical profiles in the upper atmosphere. With evidence of climate change impacts on the middle and upper atmosphere, monitoring and understanding trends through observational data is critical. There has been a contraction of the stratosphere and a decrease in the density of the upper atmosphere, which could impact the accumulation of space debris. 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 ~ 20 km to 180 km of the middle atmosphere and MLT regions, including long-term climatic changes.

The Earth's ionosphere and thermosphere form a coupled system, influenced by solar activity and magnetospheric processes from above, as well as by upward propagating disturbances from the lower atmospheric layers. This open session is intended for contributions on all aspects of ionospheric and thermospheric physics, ionospheric disturbances of different origin, and their effects on modern human technologies. The session invites theoretical studies, 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 climate. Contributions dealing with magnetospheric forcing are sought in the areas of ionospheric disturbances caused by CME- and CIR/CH HSS-related magnetic storms and substorms. New results that focus on multi-instrumental ground-based and satellite investigation of latitudinal, seasonal, and hemispheric differences in the disturbed ionospheric behaviour are especially appreciated. Also ionospheric effects from other sources, such as the solar terminator, solar eclipses, seismic activity, or human-made explosions, are welcome. As for lower atmosphere forcing, contributions are sought that focus on atmospheric waves, wave-wave and wave-mean flow interactions, atmospheric electricity and electrodynamic coupling processes.

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.

This session focuses on the intricate dynamics of space weather and space climate, investigating the Sun-Earth system's interactions across various timescales in the heliosphere, magnetosphere, ionosphere, thermosphere and lower atmosphere. It addresses the collective impact of phenomena such as coronal mass ejections, interplanetary shocks, co-rotating interaction regions, and solar energetic particles. Understanding and predicting these events is crucial for mitigating their effects on critical infrastructure, space-based technologies, and terrestrial systems.

The discussion encompasses the current state of space weather products, featuring forecast and nowcast services, satellite observations, the use of data assimilation for enhancing predictions, as well as the production of geomagnetic and ionospheric indices. Contributions employing a cross-disciplinary approach to advance our understanding of space weather and space climate are encouraged, particularly those addressing the impact of space weather on applications such as aviation, power grids, and space flights.

The session also highlights the significant progress in predictive capabilities over the past decade. This includes advancements in observational and modeling techniques, with a specific emphasis on challenges such as acquiring real-time, observation-based data, tracking solar wind transients, and evaluating predictive models. Presentations will showcase ongoing observational and modeling work, offering insights into the current landscape of space weather forecasting and potential future opportunities. By providing a comprehensive overview, the session aims to guide future scientific efforts and inform strategic planning for space missions in the dynamic field of space weather.

The new trend of artificial intelligence (AI) application in space weather and space climate has shed light on capturing the new features and the associated physical mechanisms in ionosphere and thermosphere. Generally, machine learning, especially deep learning, has been adopted in upper atmosphere modeling, resolution reconstruction and forecasting. One challenge is to make precise nowcast and forecast of ionosphere/thermosphere responses to the geomagnetic perturbations and storms, as well as other solar activities.

This session aims to address the current studies on a wide range of topics on the ionosphere/thermosphere modeling (physical, empirical,data-driven models), spatial and temporal estimation and forecast with both machine learning and deep learning methods. Furthermore, the session will cover the novel discoveries in ionosphere responses to geomagnetic perturbations and storms, new AI based methods on ionosphere/thermosphere related studies in recent two solar cycles, as well as the limitations of current AI networks and frameworks. Presentations on the observation, modeling and data science relevant to these topics are welcome.

Disk-integrated solar irradiance is the primary input of energy to the Earth climate system. Precise estimates of the absolute irradiance and how it varies are essential for understanding the dynamics of the Earth’s atmosphere. The Sun’s spectrum changes on all timescales, from seconds for space weather events to climate-relevant periods of centuries or longer.
Moreover, for understanding the state of the Earth's climate, the Earth Energy Imbalance (EEI) is the key parameter. It is the global annual mean difference between the incoming solar and reflected solar and emitted terrestrial radiation. A positive EEI corresponds to the heat continuously accumulated in the Earth's climate system – mainly the oceans, and which will - with a time delay - cause the global warming of the surface and the atmosphere. The exact knowledge of the EEI and its trend is key for a predictive understanding of global warming and assessing the efficiency of global carbon reduction policies. To determine the EEI with higher accuracy and stability, independent measurement approaches are required.
We invite contributions describing recent successes in solar irradiance observations, composite datasets, calibration reanalysis, and modelling the solar atmosphere. Measurement concepts with an emphasis on space observations, but also ground-based and in-situ measurements, as well as modeling efforts that help to better determine the energy storage in the Earth's system and the terrestrial outgoing radiation are also warmly welcome.

Over the last 20 years, numerous spacecraft have been launched into near-Earth space. In particular, the Low Earth Orbit (LEO) is becoming an increasingly popular destination for new missions. There are many advantages of utilizing the LEO orbit, such as the relatively low launch costs, close proximity to the Earth – crucial for studying the atmosphere-ionosphere system, as well as for geomagnetic field observations – and a more rapid turnover of spacecraft which allows to keep up with state-of-the-art technology. The LEO orbit is now home to over 3000 satellites, and the total number of spacecraft is set to substantially increase in the following years. The LEO missions have provided enormous volumes of data, and offer unprecedented opportunities for transforming our knowledge of various regions and processes within the geospace.

This session focuses on the analysis and interpretation of new data sets collected by LEO satellites, including CubeSats, and their possible use for modeling and applications related to Space Weather. We invite contributions that analyze the ionosphere-thermosphere-magnetosphere system, effects of particle precipitation, and geomagnetic field measurements, among other topics. Studies using both in-situ and remote sensing observations are encouraged. This session is also open to exploring novel data sets that were previously inaccessible, including commercial data recently released to the public, as well as data sets where scientific applications arose as unintended by-products of other analyses. Studies involving multi-spacecraft analysis are particularly encouraged. Additionally, submissions related to concept and Observations System Simulation Experiment (OSSE) studies for new and planned missions are welcome.