Oxia Planum, Mars is the chosen landing site for the European Space Agency’s ExoMars Rosalind Franklin Mission (RFM), expected to launch in 2028 and land in 2030. In preparation for the mission, the landing site has been extensively characterized using orbital spectral, thermal, imaging, and topographic datasets, revealing a complex geological record of aqueous alteration and diverse mineralogical units. Yet important questions remain regarding the site’s stratigraphy, geological evolution, mineralogy, and potential preservation of biosignatures. This session will bring together complementary approaches to understanding Oxia Planum and preparing for its exploration by RFM, including orbital and planned in situ investigations, geological and mineralogical modelling, mission-specific tools and strategies, terrestrial analogues, laboratory studies, and experimental work. We particularly welcome contributions from RFM team scientists and studies addressing geological scenarios, rover operations, drilling and sample selection, and the interpretation of future in situ measurements.

The mantles of Earth and other rocky planetary bodies may have been partly or fully molten early in their histories because of the energy of accretion, decay of short-lived radioisotopes, core differentiation, and giant impacts. These “magma oceans” played a fundamental role in early planetary evolution. Exchange between magma oceans and the atmosphere and core may have established the distribution of elements among major planetary reservoirs, while the evolution of magma oceans as they crystallized determined the initial thermal and chemical structure of planetary mantles. Understanding the magma ocean stage is therefore essential for reconstructing the initial conditions for the evolution of rocky planets and the formation of habitable environments. Furthermore, this early stage can be constrained by detecting its subtle fingerprints preserved in the geological records of Earth and other terrestrial planetary bodies and through astronomical observations of atmospheres of exoplanets with present-day magma oceans. Magma oceans have been an active topic of research as rapid developments in laboratory, computational, numerical, and observational capabilities push the boundaries of research closer to the conditions of this extreme stage of planetary evolution.
This session welcomes contributions on all aspects of magma oceans; relevant topics include magma ocean formation, the fluid dynamics and geochemistry/petrology of magma ocean evolution and crystallization, exchange between a magma ocean and other planetary reservoirs including degassing and core-mantle equilibration, and characterization of magma oceans based on evidence retained in the geological and magmatic records of planetary bodies. This session emphasizes exchange across disciplines and scales by inviting research employing a broad spectrum of experimental, observational, analytical, computational, and numerical approaches, such as laboratory experiments (e.g., diamond anvil cell, shock compression, tank fluid dynamics); geochemical and isotopic analyses of minerals and rocks; scaling and stability analyses; ab initio calculations and molecular dynamics simulations; and modeling (e.g., multiphase flow, smooth particle hydrodynamics, atmospheric chemistry). Contributions combining different techniques, comparing different planets, and making links between the magma ocean stage and observables in the planetary record are particularly encouraged.

Understanding the properties and history of the core of Earth-like planets is essential to constructing a global planetary structure and evolution model and has implications for the planet's thermal, compositional, and orbital evolution. Unraveling planetary cores' structures, dynamics, and history, however, requires a synergy between many fields of expertise, such as mineral physics, geochemistry, seismology, geodynamics, gravimetry, geomagnetism, or remote sensing. This session welcomes contributions from all the aforementioned disciplines following theoretical, numerical, observational, or experimental approaches and aims to serve as a catalyst for multidisciplinary studies of Earth and Earth-like planetary cores.

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, interaction with their fluid envelopes through outgassing and regassing, 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.

Throughout Earth’s history, large explosive volcanic eruptions and asteroid impacts have episodically perturbed the Earth system, driving major climate disruptions with profound consequences for the biosphere. These events can modify atmospheric composition, perturb Earth’s radiative balance, trigger abrupt surface cooling, weaken the hydrological cycle, alter ocean circulation and biogeochemistry, suppress terrestrial and marine productivity, and generate cascading effects across ecosystems and food webs. Such environmental changes may further shape the evolutionary trajectories of species, including humans.

One notable example is the Chicxulub impact about 66 million years ago, which generated a global impact winter and almost certainly triggered the Cretaceous–Paleogene mass extinction. Another example is the Toba supereruption about 74,000 years ago, which likely caused substantial climatic effects and may have affected human populations. However, the magnitudes, timescales, spatial patterns, and underlying mechanisms of climate and biosphere responses to major perturbations remain incompletely understood and actively debated.

This session invites contributions that investigate how major perturbations—including volcanic eruptions, asteroid impacts, and other abrupt climatic events of varying magnitudes—affect the climate system, terrestrial and marine ecosystems, and the evolution of mammals and humans across a wide range of timescales and regions. We welcome theoretical, observational, proxy-based, and modeling studies from multidisciplinary perspectives spanning volcanology, planetary science, climate science, paleoclimatology, ecology, archaeology, and paleoanthropology.

The concept of Earth as the sole body in the Solar System with liquid water that can harbor microbial life has been overturned by the discovery of multiple 'ocean worlds'. The Solar System is home to several planetary bodies with subsurface oceans of liquid water, including icy satellites such as Europa, Ganymede, Callisto, Enceladus, Titan and Triton, as well as dwarf planets like Pluto, and chief among these ocean worlds, the Earth. Furthermore, new icy and ocean worlds are being continuously discovered in other planetary systems as well. Like Earth, the exploration of these oceans includes both aspects of planetary evolution and habitability. The geodynamic role of oceans in planetary evolution is thus a crucial aspect of understanding not only planet formation, but the onset of biological activity as well. In what ways can the oceans of Earth serve as analogs for other oceans of the Solar System? What instrumentation can be implemented on the Earth now to further our understanding of these ocean worlds, and what technological advances might we expect in future exploration of subsurface liquid water environments beyond Earth?

This session focuses on analog sites, laboratory simulation, modeling, instrumentation and mission proposals. Coordination between Earth, marine and planetary science communities is encouraged, as well as emphasis on upcoming (e.g. JUICE and Dragonfly) and proposed missions (e.g. Enceladus Orbilander). Analog sites might encompass either geological or biological themes in the broader frame of habitability. Interfaces of ice-water (e.g. underside of floating ice shelfs and subglacial lakes), clathrate-water (e.g. ocean floor sediments, veins/fractures/faults, layered horizons and atmosphere particulates), seafloor-ocean, and rock-ice (i.e. glaciers) are of particular curiosity. Instrumentation includes sensors, buoys, submersibles, drilling and coring, as well as satellite instrumentation (e.g. spectrometers, magnetometers and gravimeters).

Throughout Earth’s history, large explosive volcanic eruptions and asteroid impacts have episodically perturbed the Earth system, driving major climate disruptions with profound consequences for the biosphere. These events can modify atmospheric composition, perturb Earth’s radiative balance, trigger abrupt surface cooling, weaken the hydrological cycle, alter ocean circulation and biogeochemistry, suppress terrestrial and marine productivity, and generate cascading effects across ecosystems and food webs. Such environmental changes may further shape the evolutionary trajectories of species, including humans.

One notable example is the Chicxulub impact about 66 million years ago, which generated a global impact winter and almost certainly triggered the Cretaceous–Paleogene mass extinction. Another example is the Toba supereruption about 74,000 years ago, which likely caused substantial climatic effects and may have affected human populations. However, the magnitudes, timescales, spatial patterns, and underlying mechanisms of climate and biosphere responses to major perturbations remain incompletely understood and actively debated.

This session invites contributions that investigate how major perturbations—including volcanic eruptions, asteroid impacts, and other abrupt climatic events of varying magnitudes—affect the climate system, terrestrial and marine ecosystems, and the evolution of mammals and humans across a wide range of timescales and regions. We welcome theoretical, observational, proxy-based, and modeling studies from multidisciplinary perspectives spanning volcanology, planetary science, climate science, paleoclimatology, ecology, archaeology, and paleoanthropology.

Planetary magnetospheres across the Solar System offer an exceptional opportunity to study universal plasma processes operating under fundamentally different magnetic, atmospheric, rotational and solar-wind conditions. Comparative investigations allow us to distinguish physical mechanisms that are common across planetary environments from those that are unique to individual systems, thereby advancing both fundamental plasma physics and planetary space weather.

Recent and ongoing missions, including BepiColombo, JUICE, Juno, Cassini, Arase, Cluster, MMS, THEMIS, Van Allen Probes, SMILE and complementary ground-based observations, together with advances in first-principles modelling, global simulations, data assimilation, machine learning and artificial intelligence are enabling a new era of comparative magnetospheric science.

We welcome observational, theoretical and modelling studies of planetary magnetospheres, including but not limited to:
• Particle acceleration, transport and loss
• Wave–particle interactions and plasma waves
• Radiation belts and energetic particle populations
• Magnetic reconnection and global plasma circulation
• Magnetosphere–ionosphere–atmosphere coupling
• Auroral processes and energetic particle precipitation
• Solar-wind-driven and internally driven magnetospheric dynamics
• Comparative studies of Mercury, Earth, Jupiter, Saturn, Uranus, Neptune, Mars, Venus and exoplanetary environments
• Numerical modelling, data assimilation, digital twins and machine learning
• Multi-mission analyses and future planetary exploration missions
We especially encourage contributions that bridge planetary science and solar-terrestrial physics, compare multiple planetary environments, or combine observations, theory and advanced data-driven methods. The session aims to strengthen interactions between the PS and ST communities, identify universal plasma processes across planetary magnetospheres, and stimulate new international collaborations and future mission concepts.

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 equatorial and low-latitude ionosphere is a region of profound ionospheric activity and variability, presenting significant challenges for both scientific understanding and operational prediction. Its strong day-to-day (DTD) variability, and its direct impact on the occurrence of plasma irregularities and associated ionospheric scintillations, remains a critical and highly challenging subject in space weather research.

A key obstacle to progress has been the inherent difficulty in obtaining simultaneous, comprehensive observations of the coupled ionosphere-thermosphere system. To truly characterize the sources of DTD variability and determine their relative importance, an integrated, multi-disciplinary approach is essential.

This session invites contributions that explore new and integrated pathways to address these challenges. We are particularly interested in:

· New Observations: Novel ground-based and space-based observational techniques and networks that provide critical data on the equatorial and low-latitude ionosphere-thermosphere system.
· Advanced Modeling: Physics-based and first-principles modeling efforts that seek to simulate and understand the sources of DTD variability and their nonlinear interactions.
· Data-Driven Approaches: Innovative applications of machine learning, data assimilation, and other data-driven techniques to fuse disparate data sets, uncover complex patterns, and improve forecasting capabilities.

The ultimate goal of this session is to foster a dialogue that bridges observation, theory, and application, with a focus on improving the predictability of the equatorial and low-latitude ionosphere and its irregularities across a wide range of solar, geomagnetic, and lower atmospheric conditions.

Planetary cores host a rich variety of dynamical processes related to the thermal, compositional, and magnetic evolution of Earth and other planetary bodies. Understanding core dynamics and the magnetic field generation process is key to constraining the evolution of planetary interiors. Coupling between planetary cores and surrounding solid layers can influence these dynamics, providing further constraints on planetary evolution.

Magnetic field generation in planetary cores results from flows of electrically conducting, iron-rich liquids strongly influenced by rotation and driven by a combination of thermal convection, compositional convection, and mechanical forcing. Observations of the geomagnetic field and other planetary magnetic fields represent unique windows into these flows. Numerical models and experiments can be used to understand these observations and provide constraints on dynamical regimes of planetary cores and their coupling with surrounding solid layers.

In this session, we welcome observational, theoretical, numerical, and experimental studies aimed at improving our understanding of the complex dynamics occurring in planetary cores and of the evolution of planetary magnetic fields. These include research on thermal, compositional, and mechanically forced convection in planetary cores, magnetic field generation and observation, and dynamical coupling between solid layers and planetary cores.

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, modelling, and the influence of environmental factors.
The session brings together scientists from all fields related to monitoring and modelling 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 modelling: advances in modelling of the cosmic-ray propagation through the magnetosphere and atmosphere, and their response to the Earth's surface
- Impact modelling: How can cosmic-ray monitoring support environmental models, weather and climate forecasting, agricultural and irrigation management, and the assessment of natural hazards

Rotation fundamentally shapes the dynamics of geophysical and astrophysical flows across a large range of scales and systems, from planetary and stellar interiors to oceans and atmospheres. Rotation gives rise to waves, coherent vortices, turbulent cascades, and large-scale mean flows. The interactions between these processes play an important role in the transport and mixing properties of the flow, and therefore the long-term evolution of planets, moons and stars.

This session welcomes theoretical, numerical, experimental, and observational studies addressing the dynamics of rotating or rotating-stratified flows. Topics include, but are not limited to, inertial, gravity, Rossby, and magnetohydrodynamic waves; wave turbulence; wave-mean flow interactions; coherent vortices and zonal flows; rotating convection; topographic effects; transport and mixing; transition to turbulence; and deep interior dynamics relevant to planetary cores, icy moons, gas giants, and stellar interiors.

This session focuses on the fundamental mechanisms governing rotating and rotating-stratified flows in natural systems, and welcomes studies that provide physical insight into these processes across geophysical and astrophysical contexts.

This session is complementary to the EGU session on 'Stratified Turbulence in Geophysical and Astrophysical Flows', with an emphasis on rotational effects and on the coupled dynamics of waves, vortices, turbulence, and mean flows.

The radioactive materials are known as polluting materials that are hazardous for human society, but are also ideal markers in understanding dynamics and physical/chemical/biological reactions chains in the environment. Therefore, man-made radioactive contamination involves regional and global transport and local reactions of radioactive materials through atmosphere, soil and water system, ocean, and organic ecosystem, and its relations with human and non-human biota. The topic also involves hazard prediction, risk assessment, nowcast, and countermeasures, which is now urgent important for the nuclear power plants in Ukraine, the Middle East, etc.

By combining long monitoring data (> halftime of Cesium 137 after the Chornobyl Accident in 1986, 16 years after the Fukushima Accident in 2011, and other events), we can improve our knowledgebase on the environmental behavior of radioactive materials and its environmental/biological impact. This should lead to improved monitoring systems in the future including emergency response systems, acute sampling/measurement methodology, and remediation schemes for any future nuclear accidents. Furthermore, the discharge of ALPS-treated water into the ocean, carried out as part of the decommissioning of the Fukushima Daiichi Nuclear Power Station, has attracted international attention and demonstrated that decommissioning a nuclear power plant that has suffered an accident requires a fundamentally different approach from that of a conventional decommissioning. Studies on past nuclear contamination events and other environmental radioactivity datasets are also welcome.

The following specific topics have traditionally been discussed:
(a) Atmospheric Science (emissions, transport, deposition, pollution);
(b) Hydrology (transport in surface and ground water system, soil-water interactions);
(c) Oceanology (transport, bio-system interaction);
(d) Soil System (transport, chemical interaction, transfer to organic system);
(e) Forestry;
(f) Natural Hazards (warning systems, health risk assessments, geophysical variability);
(g) Measurement Techniques (instrumentation, multipoint data measurements);
(h) Ecosystems (migration/decay of radionuclides).

Carbon and sulfur, despite their low bulk-planet abundance, are crucial to life as we know it, to mantle melting and volcanism, and to the climate (in-)stability of the Earth and beyond. Yet whilst every planet follows the same laws of chemistry, the specific roles of carbon and sulfur can play out to vastly different conclusions, as with Venus and the Earth. Clues to carbon and sulfur’s behaviour among the exoplanet population can be remotely accessed by observing their atmospheres. This session will explore the importance of these elements now and in deep time, across Earth, the Solar System, and exoplanets. We welcome new work from any discipline on carbon and/or sulfur in a range of contexts, from planet formation, mantle dynamics, and tectonics, to atmospheric chemistry and geobiology, progressing towards a cosmic picture of planetary evolution shaped by carbon and sulfur.

This session invites contributions on recent progress in the
characterisation of exoplanetary climate regimes based on
state-of-the-art theoretical modelling and inspired by observations from
JWST, CHEOPS, TESS, and other facilities. Recent observations of mineral
clouds and disequilibrium chemical tracers, such as SO₂, have provided a
deeper basis for understanding exoplanetary atmospheric processes and
are pushing the boundaries of our theoretical understanding of
exoplanetary climate regimes. The upcoming launch of PLATO, together
with the ongoing preparation of selected targets and the
characterisation of their atmospheric and climate properties, is equally
important for enabling and interpreting future PLATO observations. In
addition, phase-curve observations from CHEOPS and TESS have highlighted
the need to consider magnetically coupled atmospheric dynamics, while
PLATO will soon open another frontier in phase-curve observations.

This session aims to invite recent progress in exoplanet climate
characterisation based on a combination of observation and modelling.
The session focuses on cloud and gas-phase chemistry modelling, the
modelling of magnetic coupling in atmospheres and their observational
counterpart. Contributions from the cross-over studies of solar system
and exoplanet sciences are particularly welcomed.

This session is inspired by the upcoming PLATO launch in early 2027 and
ongoing CHEOPS-PLATO synergies, including atmospheric characterisation
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 as well as the
PLATO planetary phase curves working group.

This session focuses on what we can learn from Earth's climate for other planetary climate regimes, and vice versa.

While often exhibiting vastly different climates, present-day Earth and other planets are fundamentally governed by the same physics. Despite this overlap, the two communities still lack a lively exchange. This session aims to bridge this gap by bringing together experts from both fields. We welcome research using, e.g., analytic theory, EBMs, 1-D radiative-convective equilibrium models, idealized GCMs, cloud-resolving models, 3-D GCMs, experiments, and observations. We particularly highlight the hierarchical nature of these approaches.

Submissions may address five broad subtopics:
1) Radiation:
The spectral nature of radiation and its implications for climate (e.g., ECS), greenhouse and runaway greenhouse, snowball state, and radiative feedbacks. We believe that radiation offers many opportunities for exchange, since it frequently relies on similar, or even the same, underlying modeling assumptions and parameterizations.
2) Dynamics:
Circulation regimes and transitions between them, including non-dimensional parameter analysis. Communities using idealized aquaplanets are prominent in both fields. Topics may include the effects of gravity, rotation, instellation, atmospheric mass, and characteristic timescales; superrotation; day-night contrasts; circulation cells; or ocean dynamics (e.g., Matsuno-Gill pattern / “lobster”).
3) Convection:
Convection, convective inhibition (e.g., sub-Neptunes), cloud cover, and cloud-resolving models. The latter are at the forefront of both fields, being applied to Earth and other planets.
4) Atmospheric chemistry and aerosols:
Clouds, atmospheric chemistry (e.g., ozone, CH4), and hazes, including their spatial and temporal heterogeneity and their role in exotic climates. In particular, the global distribution of clouds, spanning vast spatial and temporal scales, remains poorly understood.
5) Observables and experiments:
Observational and experimental constraints on fundamental physics, including thermal phase curves, emission and transmission spectra, rotating tank experiments, and cloud/haze analog experiments. This aims to connect observational and experimental research with theoretical approaches, particularly pushing beyond “present-day Earth-like” conditions.

Coupling between subtopics is encouraged but not required and may emerge naturally from this session.

The bridge between Earth and other planetary bodies (icy moons, earth like planets, exoplanets, exomoons …) is smaller than you think!

Are you researching
oceanography (ocean currents and stratification, micro-neuston, biochemical fluxes...),
microbiology (extremophiles, ...),
hydrothermalism (deep-sea, chemosynthesis, ...),
astronomy (life on exoplanets, habitability),
sedimentology (traces of life, ...),
atmospheric sciences (habitability, UV-protection, climate, ...),
paleobiology (biosignature recognition, life in the extremes, ...),
science communication (outreach, what is life?, ...),
early earth (origin of life, formation of water oceans, ....),
geobiochemistry (geological cycles, ...),
limnology (physical, chemical, ... aspects of life),
formation of life,
or any other field related to astrobiology?

No matter whether you are focussing on field work, lab work, modelling, telescope data, rover data, remote sensing, ... , we want to hear about your research.

Then come and share your research with a multidisciplinary audience and help us bridge disciplines in our general goal of understanding astrobiology.
We welcome presentations from people at every career level and want to encourage early career researchers to submit abstracts.

Space weather is not only a challenge for spacecraft and technological infrastructure—it is also a human health challenge.
As human exploration moves beyond low-Earth orbit toward sustained operations on the Moon and future missions to Mars, understanding the relationship between solar activity, energetic particle environments, radiation exposure, and human physiology and survival risks becomes increasingly important.
Solar energetic particle events, galactic cosmic rays, interplanetary variability, and geomagnetic disturbances create complex, time-dependent radiation environments. For explorers and crews operating outside the protection of Earth's atmosphere and magnetosphere, these factors introduce risks that require understanding across space physics, radiation science, biology, medicine, engineering, and mission operations.
This session aims to bridge the traditional communities of space weather and life in the cosmos and establish a common framework connecting environmental observations and forecasting with biological effects and astronaut health.
We invite observational, experimental, modeling, technological, and interdisciplinary contributions addressing the chain from solar and heliospheric phenomena to radiation environments, biological responses, medical consequences, and operational countermeasures.
Topics of particular interest include:
• solar energetic particle (SEP) events and astronaut radiation exposure.
• galactic cosmic rays and cumulative health risks during long-duration missions.
• solar activity, heliospheric variability and radiation forecasting.
• radiation dosimetry and individual astronaut exposure assessment.
• space-weather forecasting for medical and operational decision-making.
• radiation alert systems and crew warning protocols.
• radiation shielding and protective strategies for spacecraft, lunar bases and planetary habitats.
• habitat and personalized approaches to mission and astronaut health monitoring.
• wearable and autonomous radiation and biomedical monitoring systems.
We particularly encourage studies that directly couple space weather and radiation environment with habitat construction, location and geology information, and biological and operational outcomes.
The session seeks to stimulate collaboration between communities that will need to work increasingly closely as human activity expands from low-Earth orbit toward space exploration.

The investigation of the surfaces and internal structures of planetary bodies provides key insights into their formation and evolution. The surfaces of planets and moons can be studied using cameras, multispectral data, geochemical measurements, and laboratory experiments. Geophysical datasets—especially seismic, gravity and (electro)magnetic observations—are key to inferring the internal structure and dynamics of terrestrial and giant planets, their moons, as well as asteroids and planetesimals.
The combination of surface observations and laboratory experiments with geophysical modeling is crucial to reconstruct the internal structure of planetary bodies and to explore the geodynamic processes that have shaped planetary surfaces and interiors. For instance, multispectral imaging and experimental analyses link remote sensing data to mineralogical and physical properties, offering insights into the composition of outer and internal shells. Gravity and magnetic data together with altimetry measurements provide constraints on the differentiation, density structure, and mechanical properties (i.e., rheology, elastic properties) of planetary interiors. Terrestrial analogs (e.g., terrestrial lava tubes, impact craters, volcanic products, tectonic structures, glaciers, subglacial lakes, etc.) are also investigated through a multidisciplinary approach that combines surface observations with modeling of magnetic and gravity data to understand the geological, volcanic, and tectonic processes across terrestrial planets and icy satellites. These complementary approaches, together with geological mapping and interpretation, provide an integrated framework for how planetary bodies formed, differentiated, and evolved.
This session focuses on the instruments, measurement techniques, modeling approaches, geological interpretation, terrestrial analogues and laboratory studies that provide important constraints on the evolution of planetary surfaces and interiors. We invite contributions addressing current methods and innovative strategies to overcome existing scientific/technical/methodological challenges. Results from past, ongoing, and forthcoming missions, integrative multi-dataset analyses, and forward-looking exploration concepts are also encouraged. The session aims to provide an overview of the latest observations, methods, and experiments that allow exploring the processes shaping planetary bodies and outline pathways for major discoveries in the coming decades.

This session addresses novel measurement, data analysis, and mission design 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, dual-use or multi-use instrument technologies, innovative measurement and analysis techniques, and creative solutions to increase science operations efficiency. Presentations are also encouraged on the use of artificial intelligence/machine learning within all aspects of planetary science: from tackling large or complex data sets or models, to the use of AI within instruments, flight systems, or mission design. Results from past successes, lessons learned, current implementations, and inventive ideas for the future are welcome.

The concept of Earth as the sole body in the Solar System with liquid water that can harbor microbial life has been overturned by the discovery of multiple 'ocean worlds'. The Solar System is home to several planetary bodies with subsurface oceans of liquid water, including icy satellites such as Europa, Ganymede, Callisto, Enceladus, Titan and Triton, as well as dwarf planets like Pluto, and chief among these ocean worlds, the Earth. Furthermore, new icy and ocean worlds are being continuously discovered in other planetary systems as well. Like Earth, the exploration of these oceans includes both aspects of planetary evolution and habitability. The geodynamic role of oceans in planetary evolution is thus a crucial aspect of understanding not only planet formation, but the onset of biological activity as well. In what ways can the oceans of Earth serve as analogs for other oceans of the Solar System? What instrumentation can be implemented on the Earth now to further our understanding of these ocean worlds, and what technological advances might we expect in future exploration of subsurface liquid water environments beyond Earth?

This session focuses on analog sites, laboratory simulation, modeling, instrumentation and mission proposals. Coordination between Earth, marine and planetary science communities is encouraged, as well as emphasis on upcoming (e.g. JUICE and Dragonfly) and proposed missions (e.g. Enceladus Orbilander). Analog sites might encompass either geological or biological themes in the broader frame of habitability. Interfaces of ice-water (e.g. underside of floating ice shelfs and subglacial lakes), clathrate-water (e.g. ocean floor sediments, veins/fractures/faults, layered horizons and atmosphere particulates), seafloor-ocean, and rock-ice (i.e. glaciers) are of particular curiosity. Instrumentation includes sensors, buoys, submersibles, drilling and coring, as well as satellite instrumentation (e.g. spectrometers, magnetometers and gravimeters).

Thermal remote sensing is an increasingly established technique employing passive sensors to deriveEarth’s surface properties from the radiation emitted in the Thermal Infrared (TIR) domain. Its main focus is the thermal state of an object or surface, together with the associated surface temperature and emissivity. These properties are relevant across geological, environmental, climatic, agricultural, biological, and engineering applications.

Recent technological advances have driven the development of TIR remote sensing: satellite sensors and data infrastructure systems can now acquire and manage large volumes of high-fidelity TIR data at a wide range of spatial and temporal resolutions. Besides airborne and ground-based systems, Unmanned Aerial Systems (UAS) are increasingly used as versatile platforms that combine high spatial resolution with flexible temporal revisit. Together with a growing catalogue of current and upcoming missions, this makes it a timely moment to take stock of where the field stands.

This session addresses established and emerging research directions in TIR remote sensing and discusses the community's upcoming challenges. We welcome contributions on new frontiers, case studies, and data-integration analysis related to:

• Geosciences: volcanoes, hydrothermal systems, geothermal potential, mineral exploration, rare earths, cryosphere.

• Climate, Urban Systems, and Ecosystems: urban heat islands, global warming impacts, ecosystem stress, forest health, fire risk assessment, water management.

• Agriculture and Precision Farming: crop stress monitoring, irrigation management, soil analysis and pest/disease monitoring.

• Technological and Methodological Innovations: new sensors for satellite, airborne, UAS and in-situ platforms, multi-platform and/or multi-sensor data integration, Cal/Val activities.

• Data Processing and Infrastructure: approaches for managing and processing large TIR datasets, data fusion techniques, advanced algorithms for atmospheric correction and temperature and emissivity separation.

Multi-disciplinary studies and contributions from Early Career Scientists are especially welcome.

Invited Speaker: Sabine Chabrillat, Helmholtz Centre for Geosciences (GFZ).

Recent advances in geophysical observations, numerical simulations, remote sensing products, and high-performance computing are generating large and increasingly complex multidimensional datasets. Interpreting these datasets requires advanced processing and modelling together with effective methods for visualisation and integration.
This session focuses on the development and application of advanced visualisation methods for geophysical data. We particularly welcome approaches that improve the exploration and interpretation of multidimensional, multiscale, and time-dependent datasets, and that can improve geophysical interpretation and its practical application.
We welcome contributions addressing interactive visualisation, 3-D and 4-D representations, data fusion, and the integration of observational, experimental, and modelled data. Contributions combining geophysical data with artificial intelligence and machine learning, including AI-assisted visual analytics and interactive approaches for navigating large and heterogeneous datasets, are particularly encouraged.
The session will also consider practical applications of advanced visualisation across different operational and scientific scenarios. Examples include geophysical applications in engineering and infrastructure monitoring, environmental protection and assessment, natural hazard monitoring and early-warning systems, and the management and interpretation of large and heterogeneous datasets. We also welcome applications to planetary exploration, where observations acquired by spacecraft, landers, rovers, and orbital platforms need to be integrated with geological, geophysical, topographic, and numerical datasets to investigate planetary environments.
By bringing together developments across geophysics, engineering, environmental sciences, natural-hazard research, data science, and planetary exploration, the session will provide a forum to discuss how advanced visualisation can improve the interpretation of complex geophysical datasets and support more effective, transparent, and interactive approaches to understanding the Earth and planetary geophysics.

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 the collection of BUGS - ranging from clay bricks to atmospheric temperature extremes - at https://meetingorganizer.copernicus.org/EGU25/session/52496