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 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

ESA/NASA's mission Solar Orbiter was launched in February 2020, and the in-situ instruments have started their science operations in June. The mission’s unique design will enable breakthrough science focusing on the linkage between the Sun and the heliosphere. By approaching as close as 0.28 AU from the Sun and orbiting the Sun in a plane up to 33 degrees heliographic latitude, Solar Orbiter will view the Sun and corona with remote imaging with high spatial resolution, and acquire in-situ measurements of the surrounding heliosphere. Solar Orbiter had its first perihelion near 0.51 AU in June 2020, its first Venus flyby in December and its second perihelion at 0.49 AU on 10 February 2021. Presentations covering instrument performance during commissioning and calibration, initial data and first scientific results from the first perihelia and the cruise phase (together with contextual ground and space-based observations), and theoretical predictions are solicited.

The Sun’s corona is the birthplace of the solar wind, coronal mass ejections, associated shock waves and solar energetic particles which all are fundamental drivers of space weather. The key physical processes at the origin of these phenomena, i.e. the heating and acceleration of the coronal plasma and energetic particles, have not been clarified to date. During EGU 2021 Parker Solar Probe (PSP) will go through its eight´s perihelion of its 24 scheduled orbits around the Sun. During this perihelion the spacecraft will go as close to the Sun as 15.6 solar radii. PSP has already provided a treasure trove worth of in-situ and remote sensing data. The data from the previous orbits have revealed phenomena never seen before. Solar Orbiter (SO) was successfully launched on 10 February 2020. The in-situ instruments have become fully operational and the remote sensing instruments have also been switched on. Combining the PSP observations with data from SO, with remote sensing observations from SDO, STEREO and Proba2, with other in-situ data, e.g., from ACE and DSCOVR, with ground-based observations and with theoretical models is a challenging and exciting task. This session invites scientific contributions on all aspects of research addressed to the exploration of our near-Sun environment, with special focus on the new observations from PSP and SO and other complimenting observations and models.

The majority of space plasmas are in a turbulent state, displaying fluctuations and non-linear behaviour at a broad range of scales. As well as being of fundamental interest, this turbulence may have important effects, such as heating of the solar wind and corona, acceleration of energetic particles, and interaction with magnetic reconnection and shocks. Measurements also suggest the presence of plasma instabilities which may generate quasi-linear waves, such as, e.g., Alfven-Ion-Cyclotron waves at ion scales and whistler waves at electron scales. Many aspects of the turbulence and instabilities are not well understood, in particular, the energy injection mechanism to the cascade, the non-linear turbulent cascade and dissipation mechanisms, non-linear instability saturation mechanisms, and the interaction between instabilities and turbulence. This session will address these questions though 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 Solar Orbiter and Solar Probe Plus.

Current sheets and 2D magnetic islands or 3D blobs, flux ropes, and plasmoids observed in the solar wind at various scales play a significant role in local particle acceleration to keV-MeV energies. The resulting energetic particle enhancements as well as plasma/magnetic field variations constitute a potentially hazardous condition in the interplanetary and near-Earth space. Current sheets are self-organized structures that are formed ubiquitously in cosmic and laboratory plasmas owing to a change in the magnetic field direction, at strong discontinuities, and as a result of turbulence. Not surprisingly, dynamic processes occurring at current sheets and in their vicinity have a striking similarity in different plasmas. Current sheets experience magnetic reconnection that in turn leads to many subsequent nonlinear effects, triggering the development of a turbulent cascade, the formation of magnetic islands/flux ropes/plasmoids/blobs, and local acceleration of charged particles. These processes are observed from the corona to the outer heliosphere and may often be described by the same equations. They also can be linked physically as some of the structures originating from the corona survive and evolve further in the solar wind. These processes have been studied by different scientific teams in independent ways, but currently there is a tendency to analyze them employing a unified approach.
This interdisciplinary session will bring together specialists from different plasma physics communities, bridging gaps in the understanding of the origin of coherent structures and the development of dynamical processes associated with current sheets. We invite researchers to share recent results of their theoretical studies, modelling and observations. Contributions that discuss and compare different mechanisms of local particle energization that occur in laboratory plasmas, the solar corona, magnetospheres of planets and the heliosphere are especially 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. There are challenging questions in fundamental solar system plasma physics which require the analyses of huge amounts of data, in particular of the particle kinetics. Machine learning techniques have to be used. We further encourage presentations of theory and simulation results relevant to current, forthcoming and proposed space missions. Each year a topic of special interest is chosen as a focus of the session. For 2021 this focus will be on synergies between observations in the solar wind made by Solar Orbiter and Parker Solar Probe with theory and simulation.

The solar wind is an uninterrupted flow of highly ionised plasma that fills the heliosphere and is crossed by strong transient perturbations such as 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. Remote-sensing observations from multiple vantage points, in-situ measurements from multiple well-separated locations, and novel modelling efforts have been employed systematically to study the properties of the solar wind plasma and of solar transients in general, from their formation to their arrival at different in-situ locations. However, despite the number of past and current spacecraft missions distributed throughout the heliosphere, it is still difficult to fully understand the properties of these phenomena, including their 3D structure (both global and local) and their evolution with heliocentric distance.

Studies of the ambient solar wind and its transient phenomena from their origin (the Sun) through their interplanetary journey are possible thanks to remote-sensing and in-situ observational data and models. From an observational perspective, for example, the recently launched Parker Solar Probe, BepiColombo, and Solar Orbiter have significantly increased the amount of available spacecraft in the inner heliosphere. From a modelling perspective, the recent years have seen an increase in both coronal and heliospheric models that operate in different regimes and dimensions. All these aspects will provide us with the perfect opportunity to test, validate, and refine the current knowledge of the solar wind and its transient phenomena and their interactions at different heliocentric distances. Accordingly, the aim of this session is to showcase the latest observational and modelling efforts regarding the origin and evolution of the solar wind, CMEs, and SIRs during their propagation throughout the heliosphere as seen from multiple vantage points, and to foresee future developments.

Space, laboratory, and astrophysical plasmas are seemingly different environments, which however host very similar processes: among them, turbulence, magnetic reconnection, and shocks, which all result in particle acceleration. These processes are highly non-linear, and closely interlinked. On the 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 formation, as for instance in the turbulent magnetosheath.

We are now in a fortunate time when the investigation of these processes based on simulations and observations are converging: simulations can deliver output which 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 spacecrafts. The ever growing amount of data that both simulations and observations produce can be then combed through and organized with Artificial Intelligence and Machine Learning methods.

This session welcomes simulations, 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. We also encourage papers proposing new methods, especially those rooted in Artificial Intelligence and Machine Learning, to extract new knowledge from these big observational and simulated data sets.

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., 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 (like BepiColombo, Juice, Solar Orbiter, Solar Probe, SunRISE, Taranis) are also welcome.

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. Algorithms to automatically detect and classify special features in time series data of the solar wind or in 2D images of planetary surfaces are examples of where machine learning approaches can support and improve existing models. Further, modern learning methods can encode properties of interest in lower dimensional space, and thus making them more searchable.


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.

Corona pandemic significantly affected our livies and scientific activities. All institutions, both scientific and high-education, had to find their own tips to keep the science activities. Such knowledge is often common across different scientific disciplines. This session aims to exchange such know-how. The following topics are just examples and all related contributions are welcome.

(1) How can we meet the deadlines, particularly for planetary missions with limited launch window, under corona pandemic? What are the difference between different institution and how was the result?

(2) How can we mange field works and geophysical monitoring (e.g., maintenance of instruments on sites)?

(3) Non-uniform global distribution and its time profiles of the corona pandemic suggest some geophysical (not only geographical) factors. Does geophysical condition (gradient of UV, gradient of air temperature/humidity, wind) have any correlation to the pandemic?

(4) Can we apply our analyses method on corona data? Isn't it useful to apply our multi-dimension analyses, data assimilation of different sources of data, evaluation and correction of data (and its pipeline), fractal analyses of local distribution, etc?

(5) Air pollution that reflects the human activity is known to have quickly responded to this pandemics. Are there any other geophysical monitoring method of spread and human reactions?

(6) If you or your colleague have been infected, what was the consequence to your science and science colleague

(7) What will be the optimum method to have the highest science output during corona pandemic?

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.

The Earth’s magnetosphere is significantly affected by transient solar wind features. During the interaction between the solar wind transients and the Geospace system, important energy transfer and transport occur. Solar energy in various forms can propagate into the magnetosphere and ionosphere. In the meanwhile, charged particle energy can be transformed to electromagnetic energy, and vice versa. In-depth understanding of how the magnetosphere responds to transient solar wind features will enhance our knowledge on the solar wind-magnetosphere-ionosphere coupling. 
 
 
This special session will address the processes by which solar wind mass, momentum, and energy enter the magnetosphere. Regions of interest include the foreshock, bow shock, magnetosheath, magnetopause, cusps, the dayside magnetosphere, and the dayside ionosphere. This special session will provide a forum for the latest results from in-situ spacecraft observations, ground-based observations, and global simulations. Coordinated multi-point observations are especially encouraged. Planetary dayside Magnetospheric Interaction studies are also welcome.

The state of the magnetosphere is controlled mainly by solar wind conditions. The interplanetary magnetic field (IMF) as well as solar wind plasma parameters regulate the energy input into the magnetosphere. While the IMF’s direction plays an important role in the coupling between the solar wind and magnetosphere, the questions remain on the effectiveness of the different plasma penetration mechanisms, their distribution at the magnetopause, and consequent global magnetospheric dynamics. Furthermore, the solar wind plasma parameters, such as density and velocity, may also change the magnetospheric state. There are different dynamic regimes of the magnetosphere, including the quiet magnetosphere, steady magnetospheric convection, sawtooth oscillations, substorms, and storms. It is yet unknown whether these different modes are governed by the different types of the solar wind, e.g. slow solar wind near the heliospheric current sheet, coronal mass ejections, and fast streams from coronal holes. The other open questions on the global magnetospheric dynamics include how the pre-conditioning of the magnetosphere changes its response to the solar wind impact and what are the roles of the ionosphere and ionosphere-magnetosphere coupling in the transition between magnetospheric modes.
Global magnetospheric dynamics can be studied employing numerical simulations (MHD or kinetic), using empirical and semi-empirical models, and with the help of multipoint spacecraft observations. Besides, some past and future space missions can make global magnetospheric imaging providing information about positions and dynamics of the magnetospheric boundaries and global distribution of the ionospheric currents. We welcome any work presenting results on the global dynamics of the Earth’s magnetosphere as well as other planets’ magnetospheres.

Wave-particle interactions represent a unique mechanism of an energy transfer in the nearly collisionless plasma environment of the Earth's inner magnetosphere, affecting ultimately distribution functions of energetic particles trapped in the Van Allen radiation belts. Their evaluation, along with the quantification of the resulting particle acceleration, transport, and loss, is thus crucial for understanding the dynamics of the radiation belts. Considering that these processes are mainly driven by the solar wind, the ability to accurately forecast the radiation belts is further dependent on understanding their coupling with external regions (e.g. solar wind, foreshock, magnetosheath), and the processes that dictate their global dynamics. Additionally, precipitating magnetospheric particles cause changes in the ionospheric conductivity and may affect the upper atmospheric chemistry. The aim of this session is to discuss the dynamics of energetic particle populations in the radiation belts, wave-particle interactions in the Earth's inner magnetosphere, as well as generation mechanisms and properties of involved electromagnetic emissions (EMIC, chorus, hiss, fast magnetosonic waves, etc.) in various frequency ranges (ULF, ELF, VLF). Theoretical and model contributions, as well as observational studies using data from older and recent satellite missions (Cluster, MMS, THEMIS, Van Allen Probes, ERG-Arase, etc.) and ground-based instruments are encouraged.

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 which 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. 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 a number of fascinating similarities which make comparative studies particularly interesting. We invite a broad range of theoretical, modelling, 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 modelling, 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 is composed of cold plasma that includes protons and heavy ions. This plasma can directly escape to the magnetosphere following the Earth's magnetic field lines in the polar regions, and forms the plasmasphere in the low- and mid-latitude regions. Therefore, the ionosphere is an important source that provides significant amounts of plasma to the magnetosphere and profoundly impacts its global dynamics. Depending on the path of these ions in the magnetosphere, they can end up forming cold and warm ionospheric outflows, plasmaspheric plumes, or the warm plasma cloak, and also feed the plasma sheet and ring current.

Recent simulations and observations from numerous missions, including Cluster, Van Allen Probes, THEMIS, and MMS, have sought to identify the origin, transport, and loss of plasma originating in the ionosphere and transported into the magnetosphere. These ions modify the plasma properties, and have an impact on key plasma dynamics such as wave generation and transport, particle acceleration or magnetic reconnection. This session welcomes presentations on all aspects related to ionospheric plasma in the magnetosphere. Studies based on observations, theory and simulations are encouraged.

This interdisciplinary session welcomes contributions on novel conceptual and/or methodological approaches and methods for the analysis and statistical-dynamical modeling of observational as well as model time series from all geoscientific disciplines.

Methods to be discussed include, but are not limited to:
- linear and nonlinear methods of time series analysis
- time-frequency methods
- statistical inference for nonlinear time series, including empirical inference of causal linkages from multivariate data
- nonlinear statistical decomposition and related techniques for multivariate and spatio-temporal data
- nonlinear correlation analysis and synchronisation
- surrogate data techniques
- filtering approaches and nonlinear methods of noise reduction
- artificial intelligence and machine learning based analysis and prediction for univariate and multivariate time series

Contributions on methodological developments and applications to problems across all geoscientific disciplines are equally encouraged. We particularly aim at fostering a transfer of new methodological data analysis and modeling concepts among different fields of the geosciences.

Most often observations and measurements of geophysical systems and dynamical phenomena are obtained as time series whose dynamics usually manifests a nonlinear behavior. During the past decades, nonlinear approaches in geosciences have rapidly developed to gain novel insights on fluid dynamics, greatly improving weather forecasting, on turbulence and stochastic behaviors, on the development of chaos in dynamical systems, and on concepts of networks, nowadays frequently employed in climate research.

In this short course, we will offer a broad overview of the development and application of nonlinear concepts across the geosciences in terms of recent successful applications from various fields, ranging from climate to solar-terrestrial relations. The focus will be on a comparison between different methods to investigate various aspects of both known and unknown physical processes, moving from past accomplishments to future challenges.

This session primarily focuses on the neutral atmospheres of terrestrial bodies other than the Earth. This includes not only Venus and Mars, but also exoplanets with comparable envelopes and satellites carrying dense atmospheres such as Titan or exospheres such as Ganymede. We welcome contributions dealing with processes affecting the atmospheres of these bodies, from the surface to the exosphere. We invite abstracts concerning observations, both from Earth or from space, modeling and theoretical studies, or laboratory work. Comparative planetology abstracts will be particularly appreciated.

Various space agencies around the world, the scientific community, and industrial partners are currently making advancements with a number of anticipated missions to the Moon, Mars, and other Solar System bodies. Each mission has a unique set of goals that calls for strategically selected instruments accommodating a diverse set of platforms, such as but not limited to, rovers, orbiters, and human explorers. This session invites presentations on a broad topic of future planetary missions and instruments, including those already in development. Our aim is to share latest progress, discuss preflight scientific results, and increase awareness for potential cooperation.

The Earth's ionosphere embedded in the thermosphere is a coupled system influenced by solar and magnetospheric processes from above, as well as by upward propagating disturbances from below. This open session is suitable for contributions on all aspects of ionospheric and thermospheric physics. The session invites (multi)instrumental ground-based and satellite 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 long-term variations. 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 investigation of latitudinal, seasonal and hemispherical effects of the storms and substorms on ionosphere are especially appreciated. Also results of investigation of the effects of other sources on ionospheric variability, such as solar terminator, solar eclipse, seismic activity, are welcome. As for atmospheric forcing, contributions are sought that focus on atmospheric waves, wave-wave and wave-mean flow interactions, atmospheric electricity and electrodynamical coupling processes. New results on MLT feeding (wave penetration and secondary wave generation) of ionospheric disturbances and the solar effect on the vertical propagation conditions of the atmospheric waves are welcome.

Earth’s atmosphere-ionosphere system is a stratified and vertically structured mix of gases that comprise different layers, i.e., the troposphere, stratosphere, mesosphere, and thermosphere, and its ionized part, the ionosphere. These layers are characterized by different combinations of dynamics, e.g., fluid-dynamic, chemical, and electrodynamical processes. The processes are coupled through various mechanisms, e.g., atmospheric circulations, disturbances, and various waves. The current session emphasizes the recent investigations of processes driving or reflecting vertical coupling within the atmosphere-ionosphere system in a broad range of spatial and temporal scales, such as atmospheric and ionospheric response to various waves (planetary waves, tides, gravity waves, etc.), transient phenomena (sudden stratospheric warming, seasonal transition), recurring patterns like QBO and ENSO, long-term trends in the middle and upper atmosphere and their drivers, and the relative importance of atmospheric and solar/magnetospheric forcing in the upper and middle atmosphere. This session invites contributions that discuss relevant methodologies, theory, modeling, experiment, and observations of different aspects of atmosphere-ionosphere coupling.

Plasma density irregularities can occur at all latitudes in the Earth’s ionosphere. However, the onset and evolution of these irregularities as well as their influence on the radio wave signals continue to be unsolved scientific questions. The various proposed generation mechanisms, including instability growth rates and seeding processes, are strongly coupled to the neutral atmosphere and magnetospheric dynamics, making the forecasting of ionospheric irregularities much more challenging. Recent observations from ground- and space-based measurements, as well as new innovative data analysis and modeling techniques, e.g., data assimilation and machine learning, have the potential to advance our understanding of the ionospheric irregularities. Studies that focus on the observation, modeling and prediction of plasma irregularities of different scales are welcome at this session. The mitigation of negative effects and recent developments to forecast scintillation effects on Global Navigation Satellite or other communication systems are also of high interest.

This session is devoted to the analysis of very low/low frequency (VLF/LF) techniques applied to investigate ionospheric disturbances related to natural and technological hazards. Such disturbances lasting from several milliseconds to several days can be used to study natural disasters occurring before, during and after the main event. The capability of the VLF/LF radio waves (3 kHz – 300 kHz) leads the remote sensing of the ionosphere due to the relatively low path attenuation of such frequencies allowing propagation over long distances. The purpose of this session is to provide a forum for discussion among researchers involved in studies of natural hazards like earthquakes, volcano activity, tropical cyclones and lightning, as well as in studies of technological hazards induced by high-energy solar radiation by means of VLF/LF detection system. We encourage contributions on the studies of ionospheric disturbances detected by ground-based networks like International Network for Frontier Research on Earthquake Precursors (INFREP) in Europe, South America VLF NETwork (SAVNET) in South America, World Wide Lightning Location Network (WWLLN) and others. We welcome new methods and techniques applied for the detections and the processing of the VLF/LF signals. Particular attention is given to the comprehension of the physical mechanisms at the origin of precursor signals observed before the natural hazards occurrence.

The scope of this session covers all aspects of dwarf planets and small solar system objects, e.g. comets, asteroids, dust, and meteoroids. Topics are not limited to but include dynamics, evolution, physical properties, and interactions. You are invited to present results obtained from space missions, observations, laboratory studies, theory, and numerical simulations. This session also provides a forum for presenting future space instrumentation and research results should be presented taking into account the multi-disciplinary of the field.

Interactions between the interior and atmosphere of terrestrial planets are modulated by the planets’ bulk composition, which in turn is linked to the chemical properties of their host stars. As stellar photosphere and planetary atmosphere can be directly probed, compositional properties of the rocky interior can only be inferred from other data. What constraints can be placed on the range of possible compositions of terrestrial exoplanets? How do surface-interior interactions shape atmospheric properties of rocky worlds around other stars? How diverse is the physical and chemical parameter space of these exo-worlds? We invite contributions - from geodynamics, geochemistry, cosmochemistry as well as astrophysics - that explore physical and chemical links between stars and planets and between rocky interior and atmosphere, and their implications for planet long-term evolution.

Advances in the field of cosmochemistry place important constraints on the formation and dynamical evolution of the protoplanetary disk, which complement physical modelling and astronomical observations. For example, the discovery of an isotopic dichotomy among non-carbonaceous (NC) and carbonaceous (CC) meteorites reveals the existence of early isotopically distinct reservoirs that remained isolated from each other for the first few million years of the solar system. Apart from the implications the dichotomy has for the formation and early evolution of the protoplanetary disk, it and other isotopic and chronological variations can be used to trace cosmochemical materials to their formation regions, allowing the characterization of material transport throughout solar system history. We invite contributions that propose explanations for the origin of the NC–CC dichotomy, as well as how the dichotomy relates to the timing of the formation of Jupiter (and other giant planets), the dynamics of terrestrial planet formation and radial transport in the disk, and the origin and nature of the feed stocks of Earth and Mars.

This joint session invites papers that are related to the mesosphere and lower thermosphere. It addresses the topical fields of the PRESTO (Predictability of the Solar-Terrestrial Coupling) program initiated by SCOSTEP, focusing on the role of the sun and the middle atmosphere/thermosphere/ionosphere in climate and space weather. Contributions studying radiation, chemistry, energy balance, atmospheric tides, planetary waves, gravity waves, neutral-ion coupling, and the interaction of the various processes involved are welcome. This includes work on model data as well as measurements from satellites and ground based platforms such as ALOMAR.

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. However, so far, the EEI could not be determined as the measurements were not sufficiently accurate. This calls for improved instrument technologies as well as a traceable calibration chain of the space instrumentation. In this session we invite contributions on the both the measurement of solar irradiance as well as the Earth outgoing radiation which ultimately aim to pave the way to determine EEI from space.

Space weather and space climate 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. Being able to predict (forecast and nowcast) the extreme events and develop the strategy for mitigation 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 space weather events in order to avoid failure of the critical infrastructures.

This session aims to address both the current state of the art of space weather products and new ideas and developments that can enhance the understanding of space weather and space climate and its impact on critical infrastructure. We invite presentations on various space weather and space climate-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 space weather effects on applications (e.g. on airlines, pipelines and power grids, space flights, auroral tourism, etc.) in the Earth’s environment are also welcomed.

Coronal mass ejections (CMEs), interplanetary shocks, corotating interaction regions (CIRs) and solar energetic particles (SEPs) drive heliospheric variability, causing various interplanetary as well as planetary disturbances. 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.

Originally the term ‘space weather’ referred to the way in which “the variable conditions on the Sun can influence, throughout space and in the Earth’s magnetic field and upper atmosphere, the performance of space-borne and ground-based technological systems and endanger human life or health”(1). In the last years it has been extended to all the objects of the Solar Systems, becoming “Planetary Space Weather”.
The different aspects of the interactions induced by the Sun with the many objects of the Solar System should be studied in comparison with the Earth case, to help understanding the processes involved. In fact, possible comparative studies have already proven to be a powerful tool in understanding the different effects and interactions of space weather occurring around all the bodies of the Solar System.
In the present session, we welcome abstracts from all planets’ upstream solar wind activities and their relation to planetary space weather, including especially magnetized bodies (like Mercury, the Earth, Saturn and Jupiter) as well as comparisons with unmagnetized bodies (Mars and Venus).
Since in these years many operative missions have among their science goals the planetary space weather, such as BepiColombo that will have soon two Venus Flybys and then six Mercury flybys, or Solar Orbiter that will have diverse Venus flybys as well, special focus of this session will be on Venus and Mercury and on the possible studies related to multi spacecraft observations.
In this frame, we welcome studies on:
• magnetosphere-ionosphere coupling dynamics (and auroras where present);
• the solar wind interaction with planets and moons
• inter-comparisons of planetary environments;
• observations of space weather effects from space probes and Earth-based instrumentation;
• theoretical modeling and simulations, especially in view of measurement analysis and interpretation;
• potential impacts of space weathering on technological space systems.

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. They 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.

The Earth’s magnetic field is continuously monitored by a large number of geomagnetic observatories and satellites in low Earth orbit. The use of these measurements can play a significant role in the space weather era. They can be used to monitor space weather events, such as magnetic storms, substorms and geomagnetically induced currents, and furthermore they facilitate studies of dynamic solar-terrestrial events and of their interactions. These measurements can also be used to model the magnetic field of external origin which poses presently the largest problem for progress in geomagnetic field modeling.
The aim of this session is to collect new ideas and results on how magnetic field measurements (from geomagnetic observatories and satellites such as CHAMP, Swarm, CSES, ePOP and so on) can improve our knowledge in the space weather domain.