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.

Much of our knowledge about the large-scale structure and variations of
the solar wind, interplanetary magnetic field (IMF), transients (coronal
mass ejections, shocks) and energetic particles in the inner heliosphere
(< 2 AU) was gained from multi-spacecraft in-situ measurements,
especially from missions such as Helios and STEREO as well as
conjunctions between spacecraft at various planets. We have also gained
some knowledge of structures and variability in the interplanetary space
associated with turbulence, waves and instabilities on much smaller
scales thanks to ACE, Wind and ARTEMIS as well as MMS, while their
properties on intermediate (meso) scales is yet mostly unknown. The aim
of this session is to discuss progress in our understanding of CMEs,
CIRs, shocks, SEPs, the IMF and solar wind made thanks to
multi-spacecraft measurements on various scales ranging from a fraction
of an earth radius to 1 AU and the way forward. This session invites
abstracts related to analyses and simulations of multi-spacecraft
measurements in the inner heliosphere. It is especially interested in
in-situ measurements made possible by STEREO (which will be within 60
degrees of the Sun-Earth line by the end of 2020), Solar Probe, Solar
Orbiter and missions near L1, planetary missions (MESSENGER,
BepiColombo, MAVEN) as well as future missions, concepts and
instrumentation to investigate the various scales in interplanetary
space.

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. By EGU 2020 Parker Solar Probe (PSP) will have completed the fourth of its 24 scheduled orbits around the Sun. The first three orbits have the same perihelia of 35.6 solar radii, while it will move as close as 27.8 solar radii to the Sun during the fourth and fifth orbits. PSP is providing a treasure trove worth of in-situ and remote sensing data. The data from the first two orbits, that become public on November 12, 2019, have already revealed phenomena never seen before. Solar Orbiter (SO) is scheduled to launch in February 2020. The in-situ instruments will become fully operational by May 2020. The remote sensing instruments will be switched on later. 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 will be a challenging and exciting task. This session invites oral and poster 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 topics related to the latest status of the SO mission.

With discoveries of the past (e.g., Mariner, Pioneers, Ulysses) and the present (e.g., Voyager, SOHO/SWAN, IBEX, New Horizons) heliospheric missions, the exploration of the heliosphere, its boundary regions, the outer reaches of our solar system, as well as the Very Local Interstellar Medium (VLISM) has profoundly changed the view of our space in the universe. The Interstellar Mapping and Acceleration Probe (IMAP) is a future space mission dedicated to study the interaction of the solar wind with the interstellar medium and the acceleration of energetic particles. These two topics are crucial for understanding the coupling between the inner and the outer heliosphere. The Interstellar Probe escaping beyond the solar-system boundaries with new measurements would be crucial to enable the new understanding and discoveries of the global heliosphere, the interstellar medium, the Kuiper Belt, the circumsolar dust disk, and the evolution of our solar system. This session focuses on advancing the understanding of the heliosphere and its interaction with VLISM as well as the groundbreaking science of interstellar exploration, instrumentation for relevant in-situ and remote measurements, and the relevant mission and spacecraft concepts.

Current sheets and magnetic islands observed in the solar wind play a significant role in local particle acceleration to keV-MeV energies, and the resulting energetic particle enhancements constitute a potentially hazardous condition in the interplanetary and near-Earth space. Current sheets of various scales 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 or flux ropes, 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.

Public information:
****************************************************************
Welcome to session ST1.7!
If you are interested in solar or space physics, especially, if you want to know more about processes related to current sheets and/or plasmoids/blobs/magnetic islands/flux ropes of various sizes and origins, you are in the right place at the right time!
Here you can find how dynamics of these structures impact magnetic reconnection, turbulence and particle acceleration from the solar corona to the outer heliosphere, and why these complex phenomena represent an important piece of the space weather puzzle.
Do not hesitate to ask questions, using the online chat opportunity below. Not all questions can be answered so far, but you will certainly get an exciting discussion. :-)

Please note that we organize a related Zoom conference on Wednesday, 2020 May 6, therefore there is an opportunity to communicate with some authors directly before or after the official EGU chat time. The program of the virtual meeting and the corresponding Zoom conference link can be found here:
https://drive.google.com/open?id=1k2uHDQnWPIHES3hXfKiy8VEYYFfyhM-8 (please copy the link to your browser to open it) .
You are welcome to attend!

Best regards,
Conveners of session ST1.7

The solar wind is an uninterrupted flow of highly ionised plasma that fills interplanetary space and is crossed by strong transient perturbations such as coronal mass ejections (CMEs), (corotating) stream interaction regions (SIRs), and solar energetic particles (SEPs). 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 planets throughout the inner heliosphere. 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 transients phenomena, including their 3D structure and their evolution with heliocentric distance.

The recently launched Parker Solar Probe, the imminent launch of Solar Orbiter, current and planned planetary missions, as well as potential future missions at L1, L5, and over the solar poles, will provide us with the perfect opportunity to test, validate, and refine the current knowledge of these physical 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 evolution of the solar wind and solar transients during their propagation throughout the heliosphere as seen from multiple vantage points, and to foresee future developments. Potential improvements to our current space weather forecasting capabilities will be highlighted.

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. Each year a topic of special interest is chosen as a focus of the session. For 2020 this focus will be on space plasma turbulence and its consequences for particle acceleration and plasma heating. 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 for to current, forthcoming and proposed space missions, notably MMS, Parker Solar Probe, Bepi Colombo and Solar Orbiter.

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 Open Session on Moon, Mars, Mercury, Venus as terrestrial planets systems aims at presenting highlights of relevant recent results through observations, modelling, laboratory and theory. Key research questions concerning the surface, subsurface, interior and their evolution will be discussed, as well as instruments and techniques from Earth and space.

Turbulence, reconnection and shocks are fundamental non-linear processes observed in solar, heliospheric, magnetospheric and laboratory plasmas. These processes are not separate, but rather appear to be interconnected. For instance, a close link exists between reconnection and turbulence. On the one hand the turbulence cascade favors the onset of magnetic reconnection between magnetic islands and, on the other hand, magnetic reconnection is able to 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.

This session welcomes simulations, observational and theoretical works relevant for the study of these non-linear phenomena. Particularly welcome will be works focusing on the link between them in a range of scale going from fluid MHD to kinetic. This year we encourage especially papers proposing new methods, especially those rooted in Artificial Intelligence (AI) and Machine Learning (ML), to extract new knowledge from big observational and simulated data sets.

Public information:
please check EGU chat for new zoom link and password

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 can be significantly affected by transient solar wind features. Important energy transfer and transport will occur during the interaction of transient solar wind features with the Geospace system. Solar energy in various forms can propagate into the magnetosphere and ionosphere. 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, and cusps, the dayside magnetosphere, and both the dayside polar and equatorial ionosphere. This special session will provide a forum to present the latest results from in-situ spacecraft observations, ground-based observations, and global simulations. Coordinated multi-point observations are especially encouraged.

Magnetic reconnection is a fundamental process in space, astrophysics and laboratorial plasmas that explosively converts magnetic energy into kinetic energy of charged particles. Thanks to recent spacecraft missions, e.g, Cluster, THEMIS, MMS, etc, and the development of the computing simulations, many new findings have been obtained last several years. Also, many important issues remain: the triggering mechanisms, quantitative aspects of the energy conversions, identification of the electron diffusion region, electron acceleration mechanisms, and so on. This session invites presentations on all of the aspects associated with magnetic reconnection from the spacecraft measurements, the simulations, laboratory experiments and the theoretical analysis.

When Coulomb collisions between particles become negligible in a plasma, the particle distribution functions do not easily relax to Maxwellian distributions, and the MHD formalism fails to appropriately describe the plasma. Several processes, including magnetic reconnection, wave-particle interactions at kinetic scales, or turbulent cascading become the dominant mechanisms for energy exchange between populations and plasma regions in this regime. The Earth's magnetosphere and magnetosheath are composed of fully ionized, collisionless, plasmas. They constitute a natural laboratory for investigating these processes, which are generally non-linear. We invite abstracts discussing the kinetic nature of the plasma processes that occur in the Earth's magnetosphere and its surroundings. We encourage studies taking advantage of spacecraft measurements (e.g., MMS, Van Allen Probes, ARASE, THEMIS, Cluster, Geotail), modelling using kinetic simulations (e.g, Particle-In-Cell, Vlasov equation solvers) as well as analytical works.

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. The direction of the IMF plays an important role in the coupling between the solar wind and magnetosphere. For example, during northward IMF conditions, the coupling is more complex, consisting of lobe reconnection as well as plasma transfer due to Kelvin-Helmholtz waves at the magnetospheric flanks. Quasi-radial IMF results in the formation of a foreshock upstream from the dayside magnetosphere, high-speed jets in the magnetosheath and magnetopause deformation. Magnetopause reconnection provides magnetic flux to the magnetotail, while substorms release magnetic energy stored within the magnetotail into the kinetic energy of accelerated particles. There are many different dynamic regimes or modes for the magnetosphere, including the quiet magnetosphere, steady magnetospheric convection, sawtooth oscillations, substorms, and storms. Transitions between these modes may result from changes in the upstream solar wind conditions, be the consequence of internal magnetospheric dynamics, and/or ionospheric feedback. As field-aligned currents couple the magnetosphere and ionosphere, the behaviours of the magnetosphere and ionosphere are closely related. 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 spacecraft observations. Besides, some past and future space missions can make global magnetospheric imaging providing information about positions and dynamics of the magnetospheric boundaries. One such example is the ESA/CSA Solar Wind Magnetosphere Ionosphere Link Explorer (SMILE) mission bringing into space the soft X-ray imager (SXI) and ultraviolet imager (UVI) as well as in situ instruments will be launched in 2023. We welcome any work presenting results on the global dynamics of the Earth’s magnetosphere as well as other planets’ magnetospheres.

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 particles 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, and IS-radars.

Electromagnetic waves permeate all regions of the planetary environments throughout the heliosphere, representing a unique mechanism of energy transfer in the nearly collisionless plasmas present. At Earth they play a fundamental role in the dynamics of the Van Allen radiation belts and ring current, being responsible for the particle acceleration, transport and loss. Planetary magnetospheres are highly variable systems, whose reactions to specific solar wind driving conditions can lead to important phenomena such as substorms. Considering that magnetospheric processes are ultimately driven by the solar wind, the ability to accurately forecast the trapped particle populations and magnetospheric dynamics is further dependent on understanding the coupling with external regions (e.g. solar wind, foreshock, magnetosheath).

The aim of this session is to discuss the generation and propagation of electromagnetic emissions in various frequency ranges (ULF, ELF, VLF), wave-particle interactions taking place, and the role of substorms in the dynamics of energetic particles trapped in the magnetospheres throughout the solar system. Theoretical and model contributions, as well as observational studies using data from recent satellite missions (Cluster, MMS, THEMIS, Van Allen Probes, ERG-Arase, etc.) and ground-based instruments at Earth as well as other planetary environments are encouraged.

This open session covers all aspects of small solar system objects, e.g., comets, asteroids, meteoroids, and dust. Topics include, but are not limited to, dynamics, evolution, physical properties, composition, detection, charging, heating, surface analysis, and further interactions. You are invited to present results obtained from space missions, remote sensing observations, laboratory studies, theory, and numerical simulations. This session also provides a forum for presenting future space missions and instrumentation. We encourage researchers with inter- and multi-disciplinary results.

Solicited contribution will be given by Stavro L. Ivanovski from National Institute for Astrophysics (Italy) on "The latest (dusty) pieces in the Rosetta story."

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 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 phenomena caused by CME- and particularly by 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. 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.

The atmosphere interacts tightly with its ionized portion, the ionosphere, through a variety of mechanisms, including thermal, fluid dynamical, radiative, electrodynamical, photochemical, and chemical processes. Different combinations of processes dominate different altitude ranges, shaping different atmospheric and ionospheric layers. Atmospheric waves, e.g., gravity waves, tides, and planetary waves, play key roles in the coupling between layers. These waves propagate typically from the lower atmosphere, which are composed of a broad spectrum, spatially ranging from few tens to thousands of kilometers and temporally ranging from few tens of minutes to days. This session invites papers that are related to these waves and their effects on the ionosphere, including modeling as well as observational and theoretical studies.

Public information:
Dear colleagues,

Welcome to session ST3.2.
Please find the program on the next page.
Note that we organize a WebEx virtual meeting at the same time. Authors could present their display through either the text-based chat channel or video/audio-based meeting. Therefore, if you cannot find the authors on the channel, please search them in the virtual meeting through the link below. To attend the meeting, one does not need any ID.

Sincerely,
The session conveners
 
###
WebEx virtual meeting
When: Friday, May 8, 2020 1:50 PM-4:50 PM Europe/Berlin.
Where: https://meetingsemea18.webex.com/meetingsemea18/j.php?MTID=m91ba2752e97b21c2c09795ebaa10a6f0
Alternative ways to join the meeting:
Meeting number (access code): 141 247 186
Meeting password: knDkpWdr283
Join from a video system or application: Dial 141247186@iap-kborn.webex.com
You can also dial 62.109.219.4 and enter your meeting number.
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The term space weather indicates physical processes and phenomena in space caused by the radiation of energy mainly from the Sun. Solar and geomagnetic storms can cause disturbances in positioning, navigation and communication; coronal mass ejections (CME) can affect serious disturbances and in extreme cases damages or even destruction of modern infrastructure. The ionosphere and the thermosphere are parts of a physically coupled systems ranging from the Earth surface to the Sun including the magnetosphere and the lower atmosphere. Therefore, conducting detailed investigations on governing processes in the solar-terrestrial environment have key importance to understand the spatial and temporal variations of ionospheric and thermospheric key parameters such as the total electron content (TEC) and the plasma density of the ionosphere, as well as the thermospheric neutral density, which are influencing the orbits of Low-Earth orbiting (LEO) satellites. To address all these interrelations and impacts, the Global Geodetic Observing System (GGOS) Focus Area on Geodetic Space Weather Research was implemented into the structure of the International Association of Geodesy (IAG).

This session will address recent progress, current understanding, and future challenges of thermospheric and ionospheric research including the coupling processes. Special emphasise is laid on the modelling and forecasting of space weather time series, e.g. EUV-, X-ray radiation and CMEs, and their impact on VTEC and electron density. We encourage further contributions to the dynamo electric field, the variations of neutral and ion compositions on the bottom and top side of the ionosphere, atmospheric gravity waves and TIDs. Furthermore, we appreciate contributions on the wind dynamo, electrodynamics and disturbances, including plasma drift, equatorial spread F, plasma bubbles, and resultant scintillation.

Another main topic is global and regional high-resolution and high-precision modelling of VTEC and the electron density based on empirical, analytical or physical data assimilation approaches, which are designed for post-processing or (near) real-time purposes.

This joint session invites papers that are related to the mesosphere and lower thermosphere. It addresses the topical fields of the VarSITI (Variability of the Sun and Its Terrestrial Impact) program initiated by SCOSTEP, focusing on the role of the sun and the middle atmosphere/thermosphere/ionosphere in climate (ROSMIC). 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.

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.

Public information:
Displays will presented in the same order as their numbering.

Guidelines, other things to know, and tips:
-the content of the chat is not recorded
-If possible, attendees might prepare their questions in advance and copy-paste them at the relevant time on the chat
-for questions: please start your answer by @authorname. If it is related to the display, please indicate the slide's number. That will help to keep track of the discussion.
-do not forget to use the comment 's function on EGU2020 website

This session addresses interactions of plasma and (charged) dust in the vicinity and on the surfaces of small solar system objects and in planetary ionospheres, including meteor phenomena. Surface interactions were observed at several different objects including Mercury, Pluto, asteroids, comets, Kuiper belt objects, and a number of moons. Sub-surface layers influence the electromagnetic field locally and, in this way, can be measured remotely. Furthermore, observed surface properties and exospheres are strongly influenced by complex interactions between the dusty/icy regolith, micro-meteoroids, the plasma environment and UV radiation. These processes in turn affect the plasma conditions of the surroundings. A particular case are the moons of the giant planets where interactions occur with the magnetospheres of their host planets. In this session we invite contributions that will move forward our understanding of electromagnetic, surface-plasma and dust-plasma interaction with (small) solar system bodies. The different topics include (but are not limited to) the physics of meteors and of dust in ionospheres, fundamental electromagnetic interactions of satellites enclosed in diverse atmospheric envelopes, the physics of plumes and their influence on the local electromagnetic fields, the electromagnetic effects of sub-surface (magma) oceans, ionospheric phenomena and space weathering of surfaces.

Public information:
The chat will be divided in two sections:
Topic 1 (14:00 until 14:50): meteors, dust and upper atmosphere
Topic 2 (14:55 until 15:45): rocky and icy bodies in the solar system

Please join us for fruitful discussions!

Solar wind transients, i.e. coronal mass ejections (CMEs), their associated interplanetary shocks and corotating interaction regions (CIRs) drive space weather throughout the heliosphere, 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 CMEs and CIRs 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 and data. This session is devoted to provide an overview of the current state of the space weather prediction of the arrival time and impact of 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. Emphasis will be placed on the multi-spacecraft and multi-instrument observational approaches, data-driven modelling, and community established evaluation measures. 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 and space climate are collective terms that describe the Sun-Earth system 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 dramatically important because space assets and critical infrastructures in the EU, 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.

Public information:
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.

08:30 - Start of chat time
08:30 - (poster) D3144 | EGU2020-18174 - Antonio Guerrero et al.
Agenda - Orals
08:36 - D3123 | EGU2020-7386 - Eelco Doornbos et al.
08:46 - D3124 | EGU2020-6646 - Jürgen Matzka et al.
08:56 - D3125 | EGU2020-22086 - Seán Blake et al.
09:06 - D3128 | EGU2020-9196 - Mihail Codrescu et al.
09:16 - D3129 | EGU2020-7702 - Elena Marshalko et al.
Agenda - Posters
09:26 - D3132 | EGU2020-7474 - Kiyonobu Sugihara et al.
09:32 - D3133 | EGU2020-7650 - Harri Haukka et al.
09:38 - D3135 | EGU2020-11371 - Guram Kervalishvili et al.
09:44 - D3137 | EGU2020-22188 - Tom Baltzer et al.
09:50 - D3138 | EGU2020-22144 - Chris Pankratz et al.
09:56 - D3141 | EGU2020-15904 - Jean-Marie Chevalier et al.
10:02 - D3142 | EGU2020-12084 - Christine Gabrielse et al.
10:08 - D3147 | EGU2020-1002 - Joana Alves Ribeiro et al.
10:15 - End of chat time

The topic will cover the wide range of the aspects of solar-terrestrial physics that deal with the effects of space phenomena on different levels of geo-space. Effects range from those observed on spacecraft related activities all the way down to Earth and to other Solar System bodies, including impacts on technological systems, human health and life in space, as well as Earth`s climate. We welcome theoretical, observational, as well as applied contributions (effects on terrestrial and geo-space environments) on all aspects of Space Weather. Special emphasis will be put on new multi-diagnostics data base and services and on construction of relevant roadmap for future Space Weather products, improvement of forecasting models, application for Space geodetic techniques such as GNSS(ground-and satellite-based), DORIS, VLBI, satellite altimetry or the GPS radio occultation missions, applications for GICs prediction, as well as contributions related to the ESA Space Situational Awareness (SSA). This session aims at merging new and existing methods of observations and diagnostics of Solar System habitats and Space Weather services, as LOFAR radio diagnostics and new investigation and application for incoming ESA exploration missions like JUICE and SOLAR ORBITER.

Data science, analytics and visualization technologies and methods emerge as significant capabilities for extracting insight from the ever growing volume and complexity of scientific data. The rapid advancement of these capabilities no doubt helps address a number of challenges and present new opportunities in improving Earth and Space science data usability. This session will highlight and discuss the novelty and strength of these emerging fields and technologies of these components, and their trends. We invite papers and presentations to examine and share the experience of:
- What benefits they offer to Earth and Space Science
- What science research challenges they address
- How they help transform science data into information and knowledge
- In what ways they can advance scientific research
- What lessons were learned in the development and infusion of these methods and technologies

The Earth's magnetic field is continuously monitored by a large number of geomagnetic observatories and satellites in low Earth orbit. In the past years, there has been a growing interest in space weather events and in particular in their potential hazard for the activities and infrastructures of a modern, technologically based society. It is on, or just above, the surface of the Earth indeed that several important practical effects of space weather events are realized. Therefore, both ground-based magnetic observatories and magnetic measurements from satellites 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.
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 and on how they can become useful for service providers, users, and critical infrastructure protection administrations.

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).
Nevertheless, a special focus of this session will be on the planet Mercury whose environment in a few years will be the main goal of the dual ESA/JAXA mission BepiColombo. Bepicolombo will perform the first of six flybys at the end of 2021, and will begin its orbiting phase in 2026. One of the two spacecraft, the Japanese MIO, is especially designed to study the magnetospheric environment. Additional instrumentation onboard the European planetary spacecraft, orbiting closer to the planet, will measure the inner magnetosphere interactions with the exosphere and the surface.
In this frame, we welcome studies on:
• magnetosphere-ionosphere coupling dynamics (and auroras where present);
• the solar wind interaction with planets and moons (nb: for smaller bodies refer to session PS2.3 and for pure studies on unmagnetized bodies refer to session PS1.2)
• 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.

(1) from US National Space Weather Plan (2000)

Public information:
Welcome to the session PS1.4-ST4.7 Planetary Space Weather.
The schedule will include 10 displays and it will start with our solicited talk by Chuanfei Dong.
Then, we will follow the order you will find in the list of displays.
To actively participate, you are supposed to have already read all the displays.
Nevertheless, to help you in participation to the session, we will introduce the authors who will briefly tell us about their research work.
Then, we will open to questions for about 10 minutes each, and authors will answer live.
If we will have still time, we will have a short general discussion at the end.
Enjoy our session then!
Valeria, Zhonghua, Philippe and Markus

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.