Science communication includes the efforts of natural, physical and social scientists, communications professionals, and teams that communicate the process and values of science and scientific findings to non-specialist audiences outside of formal educational settings. The goals of science communication can include enhanced dialogue, understanding, awareness, enthusiasm, influencing sustainable behaviour change, improving decision making, and/or community building. Channels to facilitate science communication can include in-person interaction through teaching and outreach programs, and online through social media, mass media, podcasts, video, or other methods. This session invites presentations by individuals and teams on science communication practice, research, and reflection, addressing questions like:

What kind of communication efforts are you engaging in and how are you doing it?
What are the biggest challenges or successes you’ve had in engaging the public with your work?
How are other disciplines (such as social sciences) informing understanding of audiences, strategies, or effects?
How do you spark joy and foster emotional connection through activities?
How do you allow for co-creation of ideas within a community?
How are you assessing and measuring the positive impacts on society of your endeavours?
What are lessons learned from long-term communication efforts?

This session invites you to share your work and join a community of practice to inform and advance the effective communication of earth and space science.

All science has uncertainty. Global challenges such as disaster risk, environmental degradation, and climate change illustrate that an effective dialogue between science and society requires clear communication of uncertainty. Responsible science communication conveys the challenges of managing uncertainty that is inherent in data, models and predictions, facilitating the society to understand the contexts where uncertainty emerges and enabling active participation in discussions. Uncertainty communication can play a major role across the risk management cycle, especially during decision-making, and should be tailored to the audience and the timing of delivery. Therefore, research on quantification and communication of uncertainties deepens our understanding of how to make scientific evidence more actionable in critical moments.

This session invites presentations by individuals and teams on communicating scientific uncertainty to non-expert audiences, addressing topics such as:

(1) Innovative and practical tools (e.g. from social or statistical research) for communicating uncertainty
(2) Pitfalls, challenges and solutions to communicating uncertainty with non-experts
(3) Communicating uncertainty in risk and crisis situations (e.g., natural hazards, climate change, public health crises)

Examples of research fitting into the categories above include a) new, creative ways to visualize different aspects of uncertainty, b) new frameworks to communicate the level of confidence associated with research, c) testing the effectiveness of existing tools and frameworks, such as the categories of “confidence” used in expert reports (e.g., IPCC), or d) research addressing the challenges of communicating high-uncertainty high-impact events.

This session encourages you to share your work and join a community of practice to inform and advance the effective communication of uncertainty in earth and space science.

Sitting under a tree, you feel the spark of an idea, and suddenly everything falls into place. The following days and tests confirm: you have made a magnificent discovery — so the classical story of scientific genius goes…

But science as a human activity is error-prone, and might be more adequately described as "trial and error". Handling mistakes and setbacks is therefore a key skill of scientists. Yet, we publish only those parts of our research that did work. That is also because a study may have better chances to be accepted for scientific publication if it confirms an accepted theory or reaches a positive result (publication bias). Conversely, the cases that fail in their test of a new method or idea often end up in a drawer (which is why publication bias is also sometimes called the "file drawer effect"). This is potentially a waste of time and resources within our community, as other scientists may set about testing the same idea or model setup without being aware of previous failed attempts.

Thus, we want to turn the story around, and ask you to share 1) those ideas that seemed magnificent but turned out not to be, and 2) the errors, bugs, and mistakes in your work that made the scientific road bumpy. In the spirit of open science and in an interdisciplinary setting, we want to bring the BUGS out of the drawers and into the spotlight. What ideas were torn down or did not work, and what concepts survived in the ashes or were robust despite errors?

We explicitly solicit Blunders, Unexpected Glitches, and Surprises (BUGS) from modeling and field or lab experiments and from all disciplines of the Geosciences.

In a friendly atmosphere, we will learn from each other’s mistakes, understand the impact of errors and abandoned paths on our work, give each other ideas for shared problems, and generate new insights for our science or scientific practice.

Here are some ideas for contributions that we would love to see:
- Ideas that sounded good at first, but turned out to not work.
- Results that presented themselves as great in the first place but turned out to be caused by a bug or measurement error.
- Errors and slip-ups that resulted in insights.
- Failed experiments and negative results.
- Obstacles and dead ends you found and would like to warn others about.

For inspiration, see last year's collection of BUGS - ranging from clay bricks to atmospheric temperature extremes - at https://meetingorganizer.copernicus.org/EGU25/session/52496.

Are you unsure about how to bring order in the extensive program of the General Assembly? Are you wondering how to tackle this week of science? Are you curious about what EGU and the General Assembly have to offer? Then this is the short course for you!

During this course, we will provide you with tips and tricks on how to handle this large conference and how to make the most out of your week at this year's General Assembly. We'll explain the EGU structure, the difference between EGU and the General Assembly, we will dive into the program groups and we will introduce some key persons that help the Union function.

This is a useful short course for first-time attendees, those who have previously only joined us online, and those who haven’t been to Vienna for a while!

Later this year, the joint ESA/JAXA mission BepiColombo will enter orbit around Mercury.
After the separation from their transfer module, the two orbiters MPO (Mercury Planetary Orbiter, ESA) and Mio (Mercury Magnetospheric Orbiter, JAXA) will pass through unexplored regions of the Hermean Environment.
Together with previous mission data of Mariner 10, MESSENGER, and BepiColombo swingbys along with insights from numerical modelling, we will be able to investigate, adapt, and improve our understanding of Mercury's origin, formation, composition, interior structure, and magnetospheric environment.

This session aims to bring together studies that present the state-of-the-art knowledge, and studies that explore the potential new data and approaches for future BepiColombo observations.
In particular, we invite studies that highlight the outstanding open questions the open questions about the Hermean environment, the progress made in addressing these questions, and the observations, models, and laboratory experiments needed to support further advances.

June 2021 marked a turning point for Venus exploration, with NASA and ESA selecting three new missions to the planet, scheduled for launch in the early 2030s. Moreover, other missions are in preparation, including Shukrayaan-1 (ISRO) and Venus Life Finder (Rocket Lab), along with the initial development of an atmospheric sample return mission by the Chinese Academy of Sciences. As we approach the ‘Decade of Venus’, many fundamental questions about the planet remain unanswered. Did Venus ever have an ocean? How and when did intense greenhouse conditions develop? How does its internal structure and dynamics compare to Earth's? And how can we reconstruct its geological history?

While fascinating in its own, Venus offers a unique window into the processes shaping other planets. In stark contrast to Earth, Venus is an inhospitable world, yet it serves as an important early-Earth analogue that may shed light on our planet’s history. Beyond the Solar System, Venus-like exoplanets are likely common, and many may already have been discovered orbiting other stars. More broadly, studying Venus can provide key insights into atmospheric evolution, interior dynamics, surface processes, and planetary habitability. This session aims to address the past, present, and future of Venus science and exploration, and what Venus can teach us about Earth as well as exo-Venus analogues. We invite contributions on a wide range of topics, including mission concepts, analyses of new and legacy observations, Earth-Venus comparisons, exoplanet observations, and the latest laboratory and modeling approaches to solving Venus' mysteries.

Among planetary bodies, Earth presents the strongest set of constraints, making it a particularly valuable reference for understanding planetary systems and their evolution. This session focuses on innovative research that bridges planetary sciences and Earth system studies. We invite contributions that present techniques and methodologies developed for planetary sciences applications that can be applied to advance our understanding of Earth's systems. Additionally, we encourage submissions in comparative planetary sciences that analyse multiple celestial bodies, including Earth, to gain broader insights into planetary processes.

This session aims to provide a comprehensive platform for discussing the latest advancements in lunar science, exploration, and sustainable utilization.
We will cover critical aspects of lunar science, including the deep interior, subsurface structure, surface morphology, up to atmospheric dynamics and the solar wind interaction. Such studies can make use of lunar mission data, lunar samples, meteorites, terrestrial analogues, laboratory experiments, and / or modeling efforts.
Furthermore, highlighting results from past and current space missions, this session seeks to explore innovative ideas for future exploration, including insights on forthcoming space missions and instrumentation aiming to greatly advance our understanding of the Moon in the next decades. In addition, the session will focus on identifying strategic knowledge gaps crucial for the safe and sustainable exploration of cis-lunar space and the lunar surface by astronauts.
We welcome all relevant contributions — spanning theoretical models, observational data, and experimental findings — from experts of different fields including science and engineering. As such, the session aims to foster a comprehensive dialogue on the status and future of lunar exploration.

This session welcomes all studies on Mars science and exploration. With many active missions, Mars research is as active as ever, and new data come in on a daily basis. The aim of this session is to bring together disciplines as various as geology, geomorphology, geophysics, and atmospheric science. We look forward to receiving contributions covering both past and present processes, either pure Mars science or comparative planetology (including fieldwork on terrestrial analogues), as well as modeling approaches and laboratory experiments (or any combination of those). New results on Mars science obtained from recent in situ and orbital measurements are particularly encouraged, as well as studies related to upcoming missions and campaigns (ExoMars, Mars Sample Return).

This session covers all aspects of the lunar and deep space exploration missions developed by CNSA, with a focus on the Chang’e series to the Moon and on Tianwen-1, CNSA’s first deep space mission, which successfully operated in Mars orbit and at its surface.

The Chang-E series of missions deployed a broad spectrum of Lunar science investigations, from remote sensing and in-situ measurements to lunar sample return and analysis. Since the Chang-E1 mission, CNSA has successfully launched six lunar exploration missions and brought samples back from the far and near sides of the Moon. It returned a broad harvest of scientific data addressing the formation of the Moon and its geophysical and geological properties, attracting broad interest from the international community. The next two missions, Chang-E 7 and Chang-E 8, are planned to be launched in 2026 and 2028, respectively.

CNSA’s series of deep space missions opened with the Tianwen-1 mission to Mars, launched in July 2020. It successfully achieved orbit, landed, and deployed the Zhurong rover, marking a significant milestone in space exploration. The mission comprises an orbiter and the Zhurong rover, which landed on Utopia Planitia, a large plain in Mars' northern hemisphere. The primary objectives of Tianwen-1 were to investigate the Martian surface, atmosphere, internal structure, magnetic field and geological history. Both the orbiter and rover have collected valuable scientific data, contributing to a deeper understanding of Mars. Its rich harvest of discoveries and their implications for the understanding of Mars will be presented and compared with results from other Mars missions. Tianwen-1 will be followed by two sample return missions: Tianwen-2, which has already been launched and is scheduled to return samples from a near-Earth asteroid in 2027, and Tianwen-3, planned to return samples from Mars.

This session primarily focuses on neutral atmospheres and exospheres of terrestrial bodies other than Earth. This includes not only Venus and Mars, but also exoplanets with comparable envelopes, small bodies and satellites with dense atmospheres such as Titan, and 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, modelling and theoretical studies, or laboratory work. Comparative planetology abstracts will be particularly appreciated.

The session has historically prioritised contributions from early career scientists.

Outgassing has played a fundamental role in forming and altering Earth’s atmosphere and climate, and, therefore, habitability throughout its history. From cataclysmic global outgassing events as LIP emplacements or the Great Oxidation Event to regional and local outgassing processes, the release of volatiles can drive both short- and long-term environmental perturbations and pose significant hazards to the biosphere. Beyond Earth, outgassing remains a key process influencing the evolution of other planetary bodies in our solar system, as demonstrated by volcanic activity on Venus or cryo-volcanism on a multitude of planetary bodies.

This session invites interdisciplinary contributions from geochemistry, planetary science, and geodynamics to advance our understanding of outgassing processes. We aim to explore the variability of outgassing and its role in past and present climate change, and its broader planetary implications. By integrating perspectives from Earth and planetary sciences, we welcome abstracts based on numerical, analytical and laboratory work in this interdisciplinary session.

Dynamical processes shape the Earth and other rocky planets throughout their history; their present state is a result of this long-term evolution. Early on, processes and lifetimes of magma oceans establish the initial conditions for their long-term development; subsequently their long-term evolution is shaped by the dynamics of the mantle-lithosphere system, compositional differentiation or mixing, possible core-mantle reactions, etc.. These processes can be interrogated through observations of the rock record, geochemistry, seismology, gravity, magnetism and planetary remote sensing all linked through geodynamical modelling constrained by physical properties of relevant phases.

This session aims to provide a holistic view of the dynamics, tectonics, structure, composition and evolution of Earth and rocky planetary bodies (including exoplanets) on temporal scales ranging from the present day to billions of years, and on spatial scales ranging from microscopic to global, by bringing together constraints from geodynamics, seismology, mineral physics, geochemistry, petrology, volcanology, planetary science and astronomy.

The dynamics of planetary cores and subsurface oceans represent fundamental components of planetary evolution models, contributing to the balance of heat and angular momentum, energy dissipation, and the generation of magnetic fields, which can be observed both in situ and remotely. The steering mechanisms in these fluid layers encompass a
range of processes, including slow thermal and compositional convection, as well as diurnal orbital perturbations, such as precession, nutations, librations, and tides. The resulting nonlinear dynamics present a significant challenge for both numerical and experimental approaches.

In this session, we welcome theoretical, experimental and numerical works to provide a comprehensive overview of the mechanisms governing planetary cores, subsurface oceans dynamics and the geodynamo models. This includes, but not only, rotating convection, orbitally driven flows, inertial/internal waves dynamics, zonal flows, turbulence in rotating fluids as well as dynamo processes.

The structure, dynamics, and history of iron-bearing planetary cores are critical to constrain the evolution of Earth and other planets. Seismological observations provide a picture of the core as it is today, with an increasing body of observations and data processing techniques offering new avenues to study the core on Earth, but also other bodies such as Mars. Additional information can be deduced from high pressure mineral physics which can help in understanding the underlying effects of composition, chemical, and crystalline structure on the core as it is today or during its evolution since the formation of the Earth. Finally, models of formation, dynamics, and heat transport and evolution can be built and combine observational constrains to help our understanding of the structure, dynamics, and history of planetary cores. In this session, we welcome contributions from all disciplines to provide a comprehensive overview of the current state of planetary cores from disciplines including seismology, mineral physics, geochemistry, magnetism, gravity, dynamics or other related fields.

Jupiter’s icy moons – Europa, Ganymede, and Callisto – are at the center of planetary science curiosity, particularly in the search for habitability in the solar system. In this context, ESA’s Jupiter Icy moons Explorer (Juice) is on its way to the Jovian system after its successful Venus gravity assist in August 2025 and is joined by NASA’s Europa Clipper following its launch in October 2024 and its Mars flyby in March 2025.

This session invites contributions from the science community related to these two missions’ objectives. This includes, but is not limited to, better understanding of Jupiter icy moons’ surface properties, internal structures and dynamics of their subsurface oceans, as well as implications for habitability. The session will also cover the moons’ complex interactions with the space environment and their dynamic evolution within the Jovian system. Finally, abstracts related to observations and future science opportunities during cruise are also welcome.

As we reflect on this unique opportunity of having two spacecrafts in the Jovian system at the same time, the session will highlight the scientific opportunities offered by each mission as well as by the dual-spacecraft configuration, emphasizing the synergistic potential of Europa Clipper and Juice.

Since entering orbit nearly 10 years ago in July 2016, the Juno spacecraft at Jupiter unveiled the secrets of Jupiter’s interior, atmosphere, and magnetosphere. Each orbit, Juno gets a close-in view of Jupiter using its suite of instruments. Thanks to Juno’s naturally-precessing elliptical orbit, Juno’s first extended mission allowed for close flybys of the Galilean moons Ganymede, Europa, and Io. The orbit continues to precess northward, allowing for detailed views of Jupiter’s poles, including the powerful aurora and atmospheric features such as the unique, surprisingly stable system of storms surrounding the north pole. Juno continues its exploration of Jupiter itself and its radiation belts, moons and rings. This session welcomes the full range of results from Juno and other Earth-based observations, including modeling studies, laboratory measurements, and other relevant topics for current and upcoming missions Europa Clipper and JUICE to the Jovian system.

Jupiter’s magnetosphere is one of the most dynamic and complex systems in the solar system. Juno’s mission extension is currently awaiting NASA’s decision. If selected, continued in situ and remote exploration, supported by Hubble, Hisaki, JWST, and ground-based telescopes, will further our understanding of Jupiter’s auroras and magnetospheric environment. These findings, combined with data from past missions, are reshaping our understanding of the Jovian system.

This session addresses how Juno’s discoveries advance our knowledge of auroral acceleration and wave–particle interactions, auroral phenomenology, magnetosphere–ionosphere coupling, moon–magnetosphere interaction, magnetopause structure, and plasma transport across the Jovian magnetosphere. These results provide key constraints to prepare for the next phase of Jovian exploration with ESA’s JUICE mission and NASA’s Europa Clipper. We welcome contributions highlighting Juno results, along with insights from past and future missions, to better understand Jupiter’s magnetosphere.

Saturn’s moon Titan is a fascinating and unique environment: the only planetary satellite with a dense atmosphere. This uniqueness has led to Titan being an object of intense scientific study and mission focus, with the Voyager 1 spacecraft, Cassini-Huygens and in coming years the Dragonfly mission, all targeted to make visits through flybys or landings. Titan offers diverse environments for study, including a methane meteorology leading to rivers, lakes and seas; vast world-wide dune fields; craters; mountains; and a suspected internal water ocean. In early 2025 Titan reached a milestone in its long annual cycle: the arrival of the northern Fall equinox, and the onset of southern spring. This time period is expected to bring significant changes in Titan’s atmosphere, including shifting stratospheric haze patterns, tropospheric methane monsoons, and the breakup of the southern winter polar vortex seen by Cassini during the last years of its extended mission. This time provides an ideal opportunity to look back at the data of Cassini-Huygens, explore new observations with the James Webb Space Telescope and ground-based facilities, and discuss planned investigations with Dragonfly. This session solicits work relevant to Titan across all scientific fronts and areas of technology development, and especially encourages new ideas from early career researchers, while also encompassing exciting recent results in laboratory experiments, modeling and simulations, and astronomical observations.

The interiors of outer solar system ocean-bearing moons are diverse in both governing physical processes and chemical structure. Identifying their governing physical and chemical processes is crucial in light of ongoing and future space missions’ objectives dedicated to the outer solar system, including Europa Clipper and JUICE. The importance of characterizing an ocean worlds’ interior is two-fold: (i) it reveals the physical and chemical processes that explain how this enigmatic class of celestial bodies works, and (ii) understanding these processes holds the key to explaining an ocean world’s evolution over time, its habitable potential, and the geological diversity of ocean worlds we see today. This conference session aims to bring together scientists across geophysical and chemical disciplines, to discuss our understanding of the processes governing ocean worlds, the observable expressions of these processes such that they can be constrained by spacecraft, and the effect these processes have on interior evolution and habitability.

We welcome contributions from scientists of all career stages and across a broad range of disciplines, including oceanography, planetary geology and geophysics, glaciology, and celestial mechanics, from theory, fieldwork, and laboratory experiments. We also encourage contributions that couple these and other aspects of icy world internal dynamics, with a focus on future observations by Europa Clipper and JUICE, and efforts of comparative planetology.

The icy moons of our Solar System are prime targets for the search for extraterrestrial life. Moons such as Saturn's Enceladus and Jupiter's Europa are considered potential habitats because of their subglacial water oceans, which are in direct contact with the rocks below. Titan, with its potential subsurface ocean, icy surface and methane-based weather, could provide an analogue for a primordial earth and the circumstances in which life developed. To assess the habitability and sample the oceans of these moons, several approaches are being discussed, including water plume surveys on Europa and Enceladus, as well as developing key technologies to penetrate the ice and even study the ocean itself with autonomous underwater vehicles, if the ice is thin enough. Moreover, a key aspect of habitability is linked with the geological processes acting on these moons. The main questions that this session aims to address are the following:
- What can we learn from analogue studies on Earth?
- What are the properties of the ice shell and how do they evolve?
- How will planned missions to these bodies contribute to furthering our understanding?
- What measurements should be conducted by future missions?

The goal of this multidisciplinary session is to bring together scientists from different fields, including planetary sciences and the cryosphere community, to discuss the current status and next steps in the remote and in-situ exploration of the icy moons of our solar system. We welcome contributions from analogue studies, on the results of current and past missions, planned missions, mission concepts, lessons learned from other missions, and more. Contributions bridging the cryosphere-icy moons communities are of particular interest to this session.

This session brings together researchers studying small space objects and dust in planetary atmospheres and nearby space. Topics include: (a) asteroids, comets, meteoroids, meteors, and meteorites, (b) dust charging and motion in space as well as on planetary surfaces, (c) dust detection and characterization by space instruments, including future missions.

We highlight the importance of combining different approaches: laboratory experiments, computer simulations, and observations. The goal is to better understand how these small bodies evolve, what they're made of, and how they influence space environments.

We especially welcome presentations on recent and upcoming space missions, early career scientists, and cross-disciplinary research and collaborative ideas.

Phobos and Deimos, the two small and enigmatic moons of Mars, represent crucial targets for advancing our understanding of planetary system formation and evolution. Despite decades of study, their origin remains one of the most debated open questions in planetary science, with hypotheses ranging from their capture as primitive asteroids to their formation through a giant impact involving Mars. These competing scenarios carry profound implications for our knowledge of both Martian history and the processes that shaped the early Solar System. From an observational perspective, Phobos and Deimos stand out as some of the darkest and most spectrally red objects known, yet no analog materials identified on Earth or elsewhere have been able to reproduce their unique spectrophotometric properties. This raises fundamental questions about their composition, surface alteration processes, and potential connections to other classes of small bodies.
This session aims to bring together contributions from diverse disciplines—remote sensing, laboratory experiments, numerical modeling, and mission science—with the common goal of investigating the physical and compositional properties of the Martian moons. Topics of interest include, but are not limited to, visible and infrared observation, surface morphology, regolith properties, thermal behavior, and space weathering processes. Special attention will also be given to recent and upcoming datasets from spacecraft observations, as well as to new mission concepts and instrument developments designed to explore these enigmatic satellites. By fostering interdisciplinary dialogue, the session seeks to advance our understanding of Phobos and Deimos and to place them in the broader context of planetary formation and evolution across the Solar System.

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

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.

The interaction of the solar wind with planetary environments generates a variety of perturbations, such as electromagnetic disturbances, energetic particle events, and surface sputtering. Various past and ongoing missions have revealed different processes of interplanetary plasma interaction with different planets and allowed for comparative investigations of planetary space weathers and space climates.

The magnetospheres, ionospheres, and upper atmospheres of planets and moons are also governed by additional sources of variability that are even less understood: atmospheric waves (i.e., tides, gravity waves, planetary waves…) propagating into upper atmospheres “from below” and, for giant planets, the exhaust gases and plasmas generated by active moons (Io in the Jovian magnetosphere, Enceladus at Saturn, Triton at Neptune etc.). These processes that find their sources in dense planetary atmospheres and moons add variable mass, momentum, and energy to their host planet's plasma environment.

A key challenge for space science is understanding both the individual effects and the complex interplay of these sources, which collectively shape the unique space weather and climate of each planet. This session will address these fundamental processes, including:
(a) solar wind and energetic particle interaction with planets, moons, asteroids and comets
(b) impacts of atmospheric dynamics and its variability on upper atmospheres and ionospheres
(c)impacts of the dynamics and variability of active moons on their host magnetosphere
(e) plasma interactions with exospheres, dust and surfaces
(f) surface space weathering
(g) potential impact of planetary environment on technological space systems
(h) inter-comparisons of planetary environments

Geophysical and astrophysical flows in stratified media exhibit stratified turbulence that gives rise to a variety of flow phenomena spanning a range of spatial scales from the Kolmogorov to planetary scales. Stratified turbulence significantly influences the flow dynamics on various temporal scales via complex nonlinear interactions, which continue to be challenging to understand, diagnose, and quantify from both theory and numerics. This understanding is fundamental to advance our knowledge of turbulent flow dynamics, and a prerequisite for improved turbulent closures and parameterizations for robust predictions of weather and climate. This session aims at bringing together the recent advancements in the field of fluid dynamics, with a focus on geophysical and astrophysical flows, as well as magneto-hydro dynamics.

Our session invites fundamental and applied contributions on stratified turbulence in fluids from theoretical, numerical, and experimental observational perspectives. The topics include, but are not limited to: two dimensional, three dimensional, isotropic, and anisotropic turbulence; regime transitions and energy cascades in turbulent flows; turbulent fluxes and transports; turbulent decay, mixing, and dissipation; stable atmospheric boundary layer flows and intermittent turbulence; wave-vortex dynamics in various turbulent regimes; wave turbulence; clear air turbulence; turbulence in weakly and strongly stratified flows and stratified shear flows.

We particularly encourage participation from early career researchers.

This session focuses on the non-linear processes taking place in space, laboratory, and astrophysical plasma. In many cases, these processes are not separated but appear interlinked. For instance, magnetic reconnection is an established ingredient of the turbulence cascade, and it is also responsible for the production of turbulence in reconnection outflows; shocks can be accountable for turbulence formation, for example, in the turbulent magnetosheath, or can be efficient particle accelerators through their interaction with the ambient turbulence.

The study of these processes has seen significant progress in recent years thanks to a synergistic approach based on simulations and observations. On the one hand, simulations can deliver output in a temporal and spatial range of scales, going from fluid to electron kinetic. That is partially also due to the advent of GPU facilities that contribute to increasing computational algorithms' power in plasma physics. On the observational side, high cadence measurements of particles and fields and high-resolution 3D measurements of particle distribution functions are currently provided by the missions MMS, Parker Solar Probe, and Solar Orbiter, opening new research scenarios in heliophysics and providing a consistent amount of new data to be analysed. Furthermore, other present and future missions that will give unique plasma measurements around solar system compact objects, such as Bepi Colombo, Juice, Comet Interceptor, and HelioSwarm are demanding the development of new numerical tools for a successful interpretation of the observations.

This session welcomes simulation, observational, and theoretical works relevant to studying the abovementioned processes. We also encourage papers proposing new methods in simulation techniques and data analysis, for example, those rooted in Artificial Intelligence or those based on multi-point satellite observations.

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 leads to the transfer of energy (and other quantities, such as cross helicity and 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. In these environments, many aspects of turbulence are not well understood, in particular, the injection and onset of the cascade, the cascade itself, the dissipation mechanisms, as well as the role of coherent structures and waves. Specific phenomena such as magnetic reconnection, shock waves, solar wind expansion, plasma instabilities, wave activity and their relationship with the turbulent cascade and dissipation are under debate. The session will explore these open questions through observational, theoretical, numerical, and laboratory studies, aiming to advance our understanding of these processes. For observational studies, we welcome contributions utilizing data from a wide range of relevant spacecraft missions, including WIND, CLUSTER, MMS, STEREO, THEMIS, Van Allen Probes, and DSCOVR, with particular emphasis on recent findings from Solar Orbiter and Parker Solar Probe.

The Sun’s atmosphere is the birthplace of multi-scale magnetic activity, e.g., flares, CMEs, jets, waves, and radio emissions, that drive a variety of solar physics phenomena such as the heating and acceleration of the coronal and solar wind plasma, particle energization and transport, and space weather throughout the whole heliosphere. Parker Solar Probe (PSP) is the first spacecraft to dive deep into the solar corona. By the EGU 2026, PSP will have completed 27 orbits, including 6 perihelia as close as 9.86 solar radii. PSP reached this ultimate perihelion of 9.86 solar radii first on 24 December 2024, and every 88 days afterwards. While PSP’s prime science phase spanned the rise of solar cycle 25 from solar minimum at launch in 2018 to maximum in 2024, it now samples the innermost heliosphere at the declining phase of the cycle. PSP observations have already led to fundamental paradigm-shifting insights into the processes driving the solar wind, CMEs, SEPs, dust, and other phenomena and environments, e.g., Venus. Remote sensing observations of the solar corona from within the sub-Alfvén regime yielded spectacular fine structures of coronal out- and inflows not visible from 1 au. Beyond breakthroughs in solar and heliospheric physics, PSP has facilitated discoveries in the physics of planets, asteroids, comets, and dust particles. Synergies between PSP, SolO, DKIST, and many other space- and ground-based observatories (e.g., PUNCH, SDO, STEREO, Proba2/3, ACE, WIND, DSCOVR, and BBSO) and with theoretical models promise a wealth of further exciting findings. In this session, we welcome contributions to all aspects of research addressed to exploring the inner heliosphere and solar corona, with a particular focus on the new observations from PSP’s closest approaches with complementary observations and models.

Understanding plasma energisation and energy transport is a grand challenge of space plasma physics, and due to its vicinity, the Earth’s Magnetospheric System provides an excellent laboratory in which to investigate such processes. Fundamental processes such as shock re-formation, magnetic reconnection, turbulence, wave-particle interactions, plasma jets braking and their combination initiate and govern particle energisation and energy transport in key regions: the foreshock, the bow shock, the magnetosheath, the magnetopause, the magnetotail current sheet, and the transition region.

ESA/Cluster and NASA/MMS four-point constellations, as well as the large-scale multipoint mission NASA/THEMIS, have greatly improved our understanding of these plasma processes at individual scales compared to earlier single-point measurements. However, such missions also revealed that a key characteristic of these processes is to operate across multiple scales, ranging from the large fluid scales to the smaller kinetic scales, implying that multi-scale in situ observations are critical. Simultaneous measurements at both fluid and kinetic scales are required to resolve scale coupling and ultimately fully understand plasma energisation and energy transport processes.
Building on previous single-scale missions, the Plasma Observatory (PMO) mission represents the next generation of space plasma physics investigations. PMO is a seven-spacecraft multi-scale mission concept tailored to study plasma energization and energy transport in the Earth's Magnetospheric System simultaneously at both fluid and ion scales. These are the scales at which the largest amount of electromagnetic energy is converted into energized particles and energy is transported.
This session invites submissions on the topic of multiscale cross-scale coupling, including simulations, multi-point techniques, instrumentation, and theory. Submissions on the connection to in-situ, remote sensing, and ground-based observations are also encouraged.

The Earth’s inner magnetosphere hosts diverse charged particle populations, including the Van Allen belts, ring current, and plasmaspheric particles, with energies from eV to MeV. Interactions among these populations provide feedback mechanisms that shape magnetospheric dynamics. For example, ring current particles generate EMIC and chorus waves, which regulate radiation belt evolution through wave–particle interactions. Ring current electrons may be accelerated to relativistic energies, while the plasmasphere modulates these processes. Coupling extends beyond the magnetosphere: precipitation affects the ionosphere, while ionospheric upflows supply plasma back into the magnetosphere. Understanding these processes is vital for fundamental science and for improving space weather forecasting.

Particle precipitation into planetary atmospheres is a key heliophysical process, controlled by solar wind, magnetospheric, and ionospheric interactions. At Earth, precipitation channels energy into the upper atmosphere, producing aurora, ionospheric currents, and enhanced satellite drag. These processes demonstrate the coupling of plasma regimes and their consequences for both natural variability and technological systems. This session emphasizes a system-science perspective on precipitation across a wide range of energies and impacts. We invite studies on the roles of different drivers, the spatiotemporal dynamics of solar wind structures and geomagnetic storms, and the effects on ionospheric conductivity, atmospheric chemistry, and dynamics.

Comparative studies of outer planet magnetospheres, shaped by unique but related drivers, further highlight universal coupling processes. We welcome theoretical, modeling, and observational contributions on the dynamics of inner magnetospheres at Earth and other planets, including magnetosphere–ionosphere coupling and responses to solar wind disturbances. Relevant datasets include MMS, THEMIS, Van Allen Probes, Arase, Cluster, LEO satellites, CubeSats, Juno, SuperDARN, magnetometers, optical imagers, incoherent scatter radars, and ground-based VLF measurements.

Kelvin-Helmholtz Instability (KHI) is a fundamental plasma process driven by velocity shears, being ubiquitous in both fluids and plasmas. It has been observed in the magnetospheres of planets with (e.g. Earth, Mercury, Jupiter, Saturn) and without a magnetic field (e.g. Mars, Venus), as well as in the solar corona and solar wind at the boundary of coronal mass ejections. Contrary to neutral fluids, which are always unstable to KHI, in a magnetized environment, the magnetic field plays a crucial role acting as a stabilizer. As a driver of large-scale vortices along the boundary, KHI contributes to mass and momentum transport, enabling plasma mixing that would otherwise be limited in a highly magnetized environment. Moreover, as the instability grows, vortices become increasingly steepen and rolled-up. The nonlinear interaction of modes produces an energy cascade from the large-scale vortices to kinetic scales, where dissipation mechanisms such as wave-particle interactions and reconnection heat the plasma. The nonlinear evolution of KHI-generated vortices can trigger secondary processes or waves, such as Rayleigh-Taylor instability, lower hybrid waves, and generate thin current sheets where magnetic reconnection can occur, as well as develop a turbulent environment.
This session promotes observational, theoretical and numerical studies of KHI dynamics across different plasma environments and scales. We also welcome contributions that explore the role of KHI in solar wind – planetary magnetosphere coupling, its interconnection or competition with other processes during the onset, as well as its role in particle acceleration and plasma transport.

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.

Recent advances in the collection and analysis of large-scale datasets have led to impressive progress in modeling individual regions of the near-Earth environment from ground to several Earth radii: thermosphere, ionosphere, plasmasphere, and magnetosphere. Machine learning approaches have shown remarkable results for these complex systems. However, these geospace "spheres" are highly interconnected, with nonlinear and time-dependent interactions that may not be fully captured by models focusing on individual regions.

This session addresses the central research question:
How can we accurately model the interconnections and feedback between the thermosphere, ionosphere, plasmasphere, and magnetosphere?

We especially welcome contributions on:
- Data-driven modeling and global-scale interactions between these regions
- Combination of multiple measurement techniques, such as low Earth orbit (LEO) satellites or remote sensing.
- Identification and incorporation of external drivers for accurate modeling of the response of the near-Earth environment to space weather.
- Innovative approaches that include data assimilation, machine learning, empirical or numerical modeling.

The session aims to foster multidisciplinary collaborations toward more integrated and comprehensive modeling of the near-Earth environment.

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

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

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

This session brings together new indevelopments in the characterisation of exoplanet climate regimes based on observations with, for example, JWST and CHEOPS and also new advances in theoretical modelling triggered by new observations. E.g. JWST for the first time observed features of solid particles which have been interpreted as signatures of mineral clouds in transition spectra of gas giant exoplanets. Smaller space telescopes like TESS and CHEOPS provide equally important insight into the physics of exoplanet atmospheres. TESS, CHEOPS and JWST phase curves and secondary eclipse spectra point to the need of a magnetically coupled atmospheric gas because the observable dayside of ultra-hot Jupiters is dominated by charged particles. While all these processes have been predicted for exoplanets before they could be observed, planetary clouds and magnetic fields have been studied for solar system planets in situ with many space missions.

This session aims to present recent progress in exoplanet atmosphere characterisation based on a combination of observation and modelling. The session focuses on cloud and gas-phase chemistry modelling, the modelling of magnetic coupling and charged particles in atmospheres and how these have and can be observed. Contributions working on the cross-over of solar system and exoplanet sciences are particularly welcomed.

This session is triggered by the upcoming PLATO launch at the end of 2026 and ongoing CHEOPS-PLATO synergies, including atmospheric characterization of hot to ultra-hot Jupiters facilitated by optical observations (secondary eclipse measurements/phasecurves) that are highly complementary to JWST observations in the infrared. The session will also discuss atmosphere interpretation activities on incorporating complex 3D modelling in their data interpretation. This session is further part of the PLATO WP activities for exoplanet gas giants.

The inner solar system has three rocky terrestrial planets with substantial atmospheres. Each one is unique and each of their atmospheres differs from every other in important ways, including their composition, isotopic and interior evolution. Many questions remain unanswered despite the long history of research on the solar system. For most of its history, the Earth has been habitable, but its atmosphere and geology have evolved tremendously. The Archean Earth was very different to the modern Earth, yet it was already habitable as early as 3.7 gigayears ago. How probable was it for the Earth to stay habitable for such a long geological time? Why did Mars lose most of its atmosphere? Its small mass certainly played a role, but what role has been played by the geological processes, for instance, volcanism and magnetic dynamo? Did Venus ever have habitable conditions? If so, how long did they last and why did they disappear?

In this session, we focus on several main topics relevant for formation of habitable conditions:
– The evolution of the composition of the atmospheres of Earth, Venus, and Mars, and the role played by volcanic outgassing and planetary dynamos;
– Influence of the atmospheric escape to space from upper atmospheres on surface conditions;
– Evolving climates and possible past habitability windows for Mars and Venus.

This session is dedicated to studies of the divergent evolution of the three planets and the role played by the Sun. We aim to provide a synergetic view of the evolution of the Earth, Venus, and Mars, with contributions on planetary interiors and magnetic dynamos, and atmospheres' formation and escape being equally welcome.

In this session, we will look at transiting exoplanets, focusing on how we observe and study them, their characteristics, and their potential habitability. We want to bring together researchers who work on planetary system formation, atmospheric studies, and different observation methods. We welcome contributions on all kinds of topics, including multi-wavelength observations, data analysis, theoretical models, and new techniques in exoplanet research.

Icy ocean worlds remain compelling targets of interest for planetary science and astrobiology-focused missions. Past spacecraft missions such as Cassini and Galileo set out to study icy moons in the outer solar system and revealed the existence of liquid subsurface oceans at Enceladus and potentially Europa. The subsurface oceans of these moons are believed to be in direct contact with their rocky cores (Carr et al. 1998; Schubert et al. 2007, 2009) and to fulfil most of the criteria for habitability: liquid water, chemical building blocks, and energy sources (Hendrix et al. 2019, Cable et al. 2021). Data analysis also uncovered the presence of biologically essential elements, as well as simple and complex organic molecules in Enceladus (Khawaja et al. 2019; Postberg et al. 2018, 2023; Waite et al. 2017), making it a tantalizing focus for future spacecraft mission concepts (Cable et al. 2021, MacKenzie et al. 2021; 2022) Europa, meanwhile, is currently the target of the ongoing Europa Clipper (Pappalardo et al. 2024) by NASA and JUICE (Grasset et al. 2013) mission by ESA, showcasing its astrobiological potential.

In planetary exploration, analogue research on Earth habitats is of great importance (Yücel et al. 2025). Instrumentation development for space missions, improvement of analytical methods, and aiding in data interpretation can greatly benefit from analogue experimental input. Both Europa and Enceladus present several similarities with respect to their internal structure (e.g., a salty subsurface ocean in direct contact with a rocky core, an ice shell several km in thickness and tidal heating). Interesting interfaces exist in the interiors of these moons where rock, liquid water, brine or ice interact, potentially allowing material and energy gradients to exist, and on Earth, such interfaces modulate habitability (Hendrix et al. 2019). Indeed, understanding Earth’s environments, analogous to particular features of icy ocean worlds, could aid future space missions to better tailor their exploratory strategies.

From the classical circumstellar habitable zone to the EUV habitable zone, the possible places to look for habitable worlds depend strongly on the interplay of planetary and stellar parameters. While observations are not yet available, theoretical models help inform future observational strategies by constraining which rocky planets could maintain atmospheres, particularly ones able to support life. Models can also help identify and interpret possible biosignatures in environments different from the Solar System. In particular, they are needed to determine whether or not a potential biosignature could be abiotic in origin.

The goal of this session is to establish synergy between the theoretical and observational aspects of the search for habitable exoplanet atmospheres. We welcome contributions related to:
- Which rocky planets can retain observable atmospheres?
- Which factors can influence observations (e.g., clouds, hazes, surface conditions…)?
- Under which combinations of planetary and stellar parameters could worlds be habitable?
- Which biomarkers are observable (with current or upcoming instruments)?
- How can biosignatures be distinguished from false positives?
- What instrumental capabilities are needed to make these observations?

Impacts are likely to have played a significant role in the emergence and evolution of life. The influence of impacts on life are manifold. Firstly, impacts by asteroids, comets and meteorites might have delivered water and other vital molecules for the early evolution of life to Earth. Secondly, impacts have in the past caused mass extinction at least once, namely in the case of the End Cretaceous impact, thereby greatly influencing the evolution of life on Earth. Heavy bombardment of impacts during the Hadean age of Earth might also have delayed or repeatedly frustrated the origin of life on Earth. Impact by large bodies still pose a non-negligible threat to terrestrial life. Eve smaller impacts can have considerable ecological implications. Thirdly, impacts might have created local favourable conditions for life, especially through the creation of impact-generated hydrothermal vents, which could have persisted for a long time after the initial impact. Thus, impacts can have both a negative and positive influence on life.
On a less dramatic note, impacts and impact sites are ideal vectors to get the public interested in geology and space sciences. Many geoparks have been created around impact craters and have been used to foster public engagement in science. Amongst other themes, the proposed session will especially invite contributions concerning the following subjects:
• Impacts and the early history of the Solar System
• Impact structures as indicators of target properties and habitability
• Role of impacts in delivery and formation of the molecular building blocks for life
• Impact-generated habitats for life
• Environmental and ecological effects of impacts
• Impacts as threats for life and humankind
• Use of impact sites for geoconservation, education and outreach

Understanding the prospects of places beyond Earth to host living systems requires understanding the properties of these places themselves: what kinds of places does life need, and what is special about such places on Earth? The answers will naturally draw upon the expertise of many disciplines, including but not limited to geology, biochemistry, atmospheric physics, and astronomy. This session invites presentations from any discipline that speak to the properties of environments that could host life, from Earth and the solar system to exoplanets.

This session aims to bring together a diverse group of scientists who are interested in how life and planetary processes have co-evolved over geological time, from the Precambrian to the Phanerozoic Eon. This includes studies of how changes in paleoenvironments have influenced the evolution of complex life - including animals, plants, and marine ecosystems - and how, in turn, biological innovations have reshaped Earth system processes. We seek to link fossil records to paleo-Earth processes, highlighting the interplay between biological evolution and tectonic, magmatic, and surface processes and explore how alternating greenhouse-icehouse climates have influenced biodiversity and ecosystem structure.
As an inherently multi-disciplinary subject, we aspire to better understand the complex coupling of biogeochemical cycles and life, the links between mass extinctions and their causal geological events, how fossil records shed light on ecosystem drivers over deep time, and how tectono-geomorphic processes impact biodiversity patterns at global or local scales. We aim to understand our planet and its biosphere through both observation- and modelling-based studies. We also invite contributions on general exoplanet-life co-evolution.

This session addresses novel remote sensing and in-situ measurement approaches for the exploration of Solar System atmospheres, bodies, ring systems, and magnetospheres. It includes such approaches as the opportunistic use of spacecraft assets to acquire bonus science data, dual-use or multi-use instrument technologies, innovative measurement and analysis techniques (including the use of AI), and creative solutions to increase science operations efficiency. Results from past and current implementations, as well as “out-of-the-box” concepts for future missions and instruments, are welcome.

Deciphering the formation and evolution of planetary bodies requires a comprehensive investigation of both their surfaces and internal structures. Seismic data provide the most direct constraints on interiors, but such measurements remain scarce across the Solar System. In their absence, gravity and magnetic field observations have become fundamental for inferring the structure and dynamics of interiors of planetary bodies, spanning the Earth, Moon, and terrestrial planets to giant planets, their moons, and small bodies.
The scientific return of these geophysical datasets is greatly enhanced when combined with complementary surface observations, laboratory experiments, and numerical modeling. Multi-spectral and hyperspectral imaging, together with experimental analyses, link remote sensing data to mineralogical and physical properties, offering insights into the composition of outer and internal layers. Altimetry measurements provide independent constraints on tidal responses and rotational dynamics, complementing gravity and magnetic data and offering key insights into the rheology and differentiation of the deep interior. Joint analyses of gravity and topography provide information regarding the thickness, density, and elastic properties of interior layers, while thermochemical evolution models connect present-day structures through space and time to long-term geophysical and geological processes. Together, these approaches provide a more integrated understanding of how planetary bodies formed, differentiated, and evolved.
This session will focus on the instruments, measurement techniques, modeling approaches, and laboratory studies that enable robust constraints on the evolution of surfaces and interiors of planetary bodies. Contributions are invited that address both achievements and limitations of current methods, as well as innovative strategies to overcome existing challenges or combine disparate methodologies. Results from past, ongoing, and forthcoming missions, integrative analyses across multiple datasets, and forward-looking exploration concepts are all welcome. By bringing together diverse perspectives, the session aims to provide a broad and technically rigorous overview of the methods by which we can infer the processes shaping planetary bodies and to outline pathways for major discoveries in the coming decades.

The session Multidisciplinary Planetary Studies and Exploration Network promotes an international and cross-disciplinary dialogue on the new frontiers of planetary sciences. We welcome contributions addressing:
a) multiscale investigations of soils and subsurfaces aimed at identifying water, ice, mineral resources, and potential natural shelters, as well as studying surface and deep dynamic processes and the landscape evolution of terrestrial planets;
b) atmospheric analyses focused on assessing environmental conditions compatible with human or microbial life;
c) astrobiological studies of extremophiles and plants in extreme environments and in simulated planetary conditions;
d) examples of innovative instrumentation and research infrastructures for the analysis of soils, atmospheres, and biological systems in planetary or analogue contexts.
The overall goal is to advance our understanding of planets as integrated and living systems, in which geological, atmospheric, chemical, and potential biological processes interact within a unified picture, and to foster dialogue across disciplines. Contributions from Early Career Scientists, as well as results from experimental campaigns carried out at terrestrial analogue sites, are particularly encouraged.

Several current and near future missions include in their payload the instruments for the chemical analysis of planetary planetary soils and rocks. The proposed session will allow us to look in more details into the instrument landscape including their designs, the measurements capabilities for trace elements/isotopes and detection limits to organic and bioorganic compounds. The current instrumental performance for the detection of biomarkers and in the application to the radiometric material dating can be demonstrated.

Rocket launches and re-entries of reusable and discarded objects adds familiar and exotic anthropogenic trace gases and aerosols to all layers of the atmosphere. The space sector is the only anthropogenic source released directly to the middle and upper layers of the atmosphere. Once emitted to these layers, pollutants persist for years, leaving a long legacy of atmospheric pollution. These pollutants are increasingly ubiquitous due to recent exponential space sector growth, yet there are no regulatory controls targeting these emissions. Quantification of the complex and unique effects on the atmosphere is hindered by many uncertainties and data gaps, such as the chemical composition of exhaust from novel propellants, the resultant evolution during plume afterburning, the locations and trajectories of ablative re-entry, the radiative and chemical kinetic properties of the pollutants, and the physical and chemical evolution of controlled and uncontrolled re-entry. Lack of openly-available modelling tools is compounded by a scarcity of real-world experiments and observations, and future scenarios are hindered by a lack of commercial space activity data or well-supported growth projections. This session invites submissions across all geophysical and related disciplines in and beyond academia to share planned, current, or ongoing research that provides new knowledge in this area, explores and devises new open-source modelling techniques, or exposes methodological gaps that need to be resolved to inform sustainability initiatives and global regulation. We are also interested in innovative methods adopted by researchers in other domains that could be applied to advance understanding of environmental harm from the space sector. These include related topics such as geoengineering, space weather, space engineering, upper atmosphere circulation and chemistry, and meteors.

Stable and radiogenic isotopic records have been successfully used for investigating various terrestrial and marine sequences in term of special events including geological boundaries, fossils, evaporative rocks, palaeosols, lacustrine, loess, caves, peatlands. The session includes contributions using isotopes along with sedimentological, biological, paleontological, mineralogical, chemical records in order to unravel past and present climate and environmental changes or as tracers for determining the source of phases involved. Directions using triple isotopes, clumped isotopes, biomarkers and non-traditional stable isotopes are welcomed.
The session invites contributions presenting an applied as well as a theoretical approach. We welcome papers related to reconstructions (at various time and space scales), fractionation factors, measurement methods, proxy calibration, and verification.

Radar is a prominent tool for studying ice on Earth and is becoming widespread on other planetary bodies. In this session, we hope to bring together all those interested in radar data and analysis to showcase their work, take inspiration from each other and develop new (interdisciplinary) collaborations. We aim for this session to encompass various targets, instruments and applications, such as:

- Targets: snow, firn, land ice, sea ice, lake ice, river ice and permafrost on Earth as well as the surfaces and interiors of Mars, Europa, Ganymede, The Moon, Titan, Venus, Small bodies, etc.
- Instruments: airborne and spaceborne sounders, altimeters, SAR and passive microwave radiometers as well as drones, GPR, ApRES, pRES and other radars.
- Acquisition and processing: hardware, passive measurements, datasets, algorithm development, etc.
- Analysis and interpretation techniques: reflectometry, interferometry, thermometry, specularity, EM simulations, inversion, etc.
- Applications: investigations in surface-, englacial, subglacial and proglacial areas, scattering interfaces, roughness, hydrology, geothermal heat flux, material properties, fabric, modelling/supporting lab work, Earth and extraterrestrial analogues/synergies, etc.

We especially encourage the participation of Early Career Researchers and those from underrepresented groups.

The rapid growth of missions, observatories, and monitoring systems in the heliosphere, across the Solar System and from terrestrial or airborne facilities has created an unprecedented volume and diversity of data. Making sense of these observations requires methods that can both process large datasets efficiently and extract meaningful physical insight. Machine learning has become an important tool in this effort, complementing established physics-based approaches by enabling new ways of discovering patterns, building predictive models, and working with complex or incomplete measurements.

In recent years, increasing attention has been given to hybrid methods that combine machine learning with physical models. These approaches are now being applied across planetary and heliophysical domains, from forecasting solar eruptions and solar wind conditions, to automating the analysis of planetary surfaces or improving on-board data handling. They demonstrate how data-driven methods can benefit from physical knowledge, while physics-based models can be improved through modern data analysis techniques.

This session aims to provide an inclusive and interdisciplinary forum for researchers applying machine learning in planetary sciences and heliophysics, as well as those developing methods at the intersection between data-driven and physics-based approaches. We particularly encourage contributions that illustrate the wide range of applications, encourage exchange between disciplines and showcase the transition from research to operations.

Earth System Sciences (ESS) datasets, particularly those generated by high-resolution numerical models, are continuing to increase in terms of resolution and size. These datasets are essential for advancing ESS, supporting critical activities such as climate change policymaking, weather forecasting in the face of increasingly frequent natural disasters, and modern applications like machine learning.

The storage, usability, transfer and shareability of such datasets have become a pressing concern within the scientific community. State-of-the-art applications now produce outputs so large that even the most advanced data centres and infrastructures struggle not only to store them but also to ensure their usability and processability, including by downstream machine learning. Ongoing and upcoming community initiatives, such as digital twins and the 7th Phase of the Coupled Model Intercomparison Project (CMIP7), are already pushing infrastructures to their limits. With future investment in hardware likely to remain constrained, a critical and viable way forward is to explore (lossy) data compression & reduction that balance efficiency with the needs of diverse stakeholders. Therefore, the interest in compression has grown as a means to 1) make the data volumes more manageable, 2) reduce transfer times and computational costs, while 3) preserving the quality required for downstream scientific analyses.

Nevertheless, many ESS researchers remain cautious about lossy compression, concerned that critical information or features may be lost for specific downstream applications. Identifying these use-case-specific requirements and ensuring they are preserved during compression are essential steps toward building trust so that compression can become widely adopted across the community.

This session will present and discuss recent advances in data compression and reduction for ESS datasets, focusing on:

1) Advances in and reviews of methods, including classical, learning-based, and hybrid approaches, with attention to computational efficiency of compression and decompression.
2) Approaches to enhance shareability and processing of high-volume ESS datasets through data compression (lossless and lossy) and reduction.
3) Inter-disciplinary case studies of compression in ESS workflows.
4) Understanding the domain- and use-case specific requirements, and developing methods that provide these guarantees for lossy compression.

Geological mapping and modelling are fundamental pillars of the geosciences, providing the basis for understanding Earth and planetary systems. This session brings together contributions that span the full spectrum of geological mapping and modelling, from traditional field-based methods to cutting-edge approaches, including AI, applied in the most extreme and inaccessible environments on Earth and beyond.
We invite scientists working on:
• Geological field mapping and cross-boundary harmonization
• Mapping of extreme environments such as marine areas, polar regions, deserts, volcanic terrains, high-mountain ranges, and planetary surfaces
• 3D geological modelling in any geological context
• Development of geomodelling methodologies and tools
• Application of AI methods to geological mapping and modelling
• Development of geological information systems
• Remote sensing, geophysical techniques, drilling, sampling, and specialized tools for inaccessible terrains for geological mapping and modelling
The session aims to be highly transdisciplinary, bridging geology, geophysics, geochemistry, mineralogy, hydrogeology, engineering geology, and planetary sciences. By integrating approaches across diverse contexts, from accessible outcrops to remote and hostile terrains, participants will explore common challenges in data acquisition, interpretation, 3D modelling, visualization, and knowledge synthesis.
Outcomes are expected to benefit a wide range of applications and research, including geothermal energy exploration, offshore wind energy, geological risk assessment, groundwater protection, coastal protection, habitat mapping, environmental impact assessment, marine protected area development, mineral and resource exploration, and planetary missions. Ultimately, this session seeks to foster dialogue between communities tackling mapping and modelling challenges in both familiar and extreme environments, to advance scientific understanding and practical applications across the geosciences.

Mineral magnetism involves a wide range of laboratory and computational methods with applications in biological, geological, environmental, material and planetary sciences. Recent advances in imaging, computational modelling and experimental techniques now allow for an unprecedented level of detailed characterisation of magnetic minerals in both terrestrial and extraterrestrial materials. New mineral magnetic datasets potentially inform understanding of palaeomagnetic recording, (palaeo)climatic variability, biomineralization, planet formation and diverse modern environmental and anthropogenic processes. In this session, we welcome mineral magnetic studies across all scales with emphasis on innovative approaches that address key challenges in biological, earth, environmental and extra-terrestrial research. This will be an inclusive forum for open discussion of fundamental concepts, new methods, applications and future directions in mineral magnetism.

Research on water and ice, resources, and potential habitability on terrestrial planets of the Solar System requires innovative tools capable of probing surface and subsurface environments with high sensitivity and adaptability. These represent new challenges for planetary exploration. This session focuses on the development and application of advanced geophysical methods and on multi-platform and multi-scale technological systems designed for planetary investigations.
We welcome contributions on magnetic, electromagnetic, radar, and gravimetric techniques, as well as their integration with optical, infrared, and proximal sensing. Special emphasis is placed on scalable platforms, miniaturized instrumentation, and the cross-fertilization between terrestrial geophysical surveys and planetary missions. The goal is to foster interdisciplinary dialogue on strategies to detect water, characterize planetary crusts, assess habitable niches, and support in-situ resource utilization (ISRU). By bridging geophysics, engineering, and planetary science, this session aims to highlight the next generation of exploration tools for sustainable and scientifically rewarding robotic and human missions.

This session invites contributions on the latest developments and results in lidar remote sensing of the atmosphere, covering • new lidar techniques as well as applications of lidar data for model verification and assimilation, • ground-based, airborne, and space-borne lidar systems, • unique research systems as well as networks of instruments, • lidar observations of aerosols and clouds, thermodynamic parameters and wind, and trace-gases. Atmospheric lidar technologies have shown significant progress in recent years. While, some years ago, there were only a few research systems, mostly quite complex and difficult to operate on a longer-term basis because a team of experts was continuously required for their operation, advancements in laser transmitter and receiver technologies have resulted in much more rugged systems nowadays, many of which are already operated routinely in networks and several even being fully automated and commercially available. Consequently, also more and more data sets with very high resolution in range and time are becoming available for atmospheric science, which makes it attractive to consider lidar data not only for case studies but also for extended model comparison statistics and data assimilation. Here, ceilometers provide not only information on the cloud bottom height but also profiles of aerosol and cloud backscatter signals. Scanning Doppler lidars extend the data to horizontal and vertical wind profiles. Raman lidars and high-spectral resolution lidars provide more details than ceilometers and measure particle extinction and backscatter coefficients at multiple wavelengths. Other Raman lidars measure water vapor mixing ratio and temperature profiles. Differential absorption lidars give profiles of absolute humidity or other trace gases (like ozone, NOx, SO2, CO2, methane etc.). Depolarization lidars provide information on the shapes of aerosol and cloud particles. In addition to instruments on the ground, lidars are operated from airborne platforms in different altitudes. Even the first space-borne missions are now in orbit while more are currently in preparation. All these aspects of lidar remote sensing in the atmosphere will be part of this session.

The "Planetary Geomorphology and Surface Processes" session brings together scientists studying how landscapes form, evolve, and erode on Earth and other planetary bodies in our Solar System.
Our session will provide a platform for cross-planetary discussion of the processes that generate and erode landscapes, create stratigraphy, and couple planetary surface dynamics to climatic and tectonic drivers. Considered processes could include aeolian, volcanic, tectonic, fluvial, glacial, periglacial, or as-yet "undetermined" ones.
We welcome contributions on Mars, Venus, Mercury, the Moon, icy satellites of the outer solar system, comets, and/or asteroids, to submit to our session. We believe that an interdisciplinary approach through sharing and discussing ideas across planetary borders is key in answering current questions and for the formation of new ideas, and thus we especially encourage cross-planetary contributions. We particularly welcome contributions from early-career scientists and geomorphologists who are new to planetary science.

Studying materials and processes under extreme pressure-temperature conditions is central to understanding the interiors and evolution of Earth and Earth-like planets. Deep inside our planet, diverse physical and chemical phenomena, such as core–mantle differentiation, mantle plume origins, and enigmatic low-velocity regions, govern planetary structure and long-term evolution. Yet our direct observations—seismological, heat flux, gravity, and geomagnetic fields—leave many aspects of the deep Earth open to interpretation. Insights into mineral physics properties—such as equations of state, elasticity, texture, transport properties, phase transitions, melting, and chemical reactivity—are critical to constrain models of planetary interiors. In parallel, geodynamical modeling allows us to test hypotheses about these processes by making quantitative predictions that can be compared with observations. The scope of such studies now extends beyond Earth. Since the commissioning of the James Webb Space Telescope in 2022, exoplanet characterization has accelerated, particularly for rocky, potentially habitable planets.

Recent advances in experimental and computational techniques now allow access to an unprecedented range of conditions relevant to planetary interiors. Static compression experiments with diamond anvil cells reach pressures in the megabar regime, while dynamic compression with free-electron lasers enables ultrafast measurements at extreme conditions relevant to large exoplanets—opening unique opportunities to capture transformations of matter linked to planetary evolution. Complementary computational methods, from ab initio simulations to large-scale geodynamical models, provide key insights to predict the properties of matter at depth and link them to observable planetary parameters such as seismic velocities, mass–radius relationships, or interior dynamics.

This session invites contributions from across planetary sciences that advance our understanding of materials and processes under extreme conditions. We particularly welcome studies addressing mineral physics properties, interior structure and dynamics, and the chemical and physical evolution of Earth and exoplanets. Abstracts highlighting novel experimental techniques, innovative synchrotron and FEL approaches, and cutting-edge modeling methods can all come together to reveal the complex interplay of chemistry, physics, and dynamics within Earth and planetary interiors.

Seismic attenuation, involving energy loss through scattering and intrinsic absorption, significantly affects seismic wave propagation. As a fundamental property, attenuation plays a central role in subsurface imaging, investigations of Earth’s deep interior, and seismic exploration of planetary bodies. Quantitative analysis of attenuation enables inference of key material properties, such as composition, fluids, or fractures. A comprehensive understanding of attenuation mechanisms also supports robust source characterization and accurate ground-motion modeling, with important implications for hazard assessment and mitigation. In recent decades, advances in theory, numerical modeling, and data analysis have substantially improved attenuation characterization. High-accuracy 3D simulations now allow realistic modeling of wave propagation through complex structures, while advanced inversion techniques better separate scattering from intrinsic absorption. On the observational side, dense seismic arrays and new sensing technologies provide major, yet still underexploited, opportunities to enhance resolution.
This session will bring together experts to present the latest innovations in seismic attenuation research. We welcome theoretical and applied contributions, from work deepening fundamental understanding to studies showcasing practical applications.
Topics of interest include:
• Theoretical advancements that improve understanding of attenuation processes, including scattering and intrinsic absorption.
• Resolve Earth’s internal structure through analysis of attenuation data.
• Numerical simulations of the relevant equations for seismic wave propagation in heterogeneous media and attenuation.
• Applications to the study and characterization of seismic sources.
• Attenuation studies in seismic hazard and damage assessment, including ground motion models and the effects of shaking on structures and infrastructure.
• Energy dispersion from geological heterogeneities, such as faults, fractures, and variations in rock properties.
• Attenuation as an indicator of energy conversion into heat, with applications to geothermal exploration and volcanic hazard assessment.
• Tomographic imaging that integrates attenuation, scattering, and absorption to investigate Earth’s structure from crust to core.
• Planetary science investigations that use seismic attenuation to probe the internal structure and dynamics of other planetary bodies.