The objective of the General Session is to accommodate abstracts from a program group that do not align with the themes of any existing sessions within the same program group. Please note that all submitted abstracts may be reallocated to a different session at the discretion of the respective session chairs.

This session welcomes all presentations on Mars' interior and surface processes. 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, mineralogy, glaciology, and chemistry. We welcome presentations on both past and present processes, either pure Mars science or comparative planetology (including fieldwork on terrestrial analogues), either observations or modeling or 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 is now established for 10 years, and typically attracts a good amount of contributions reflecting the diversity of missions and science questions related to the solid portions of, covering the broad scope of current research.

Space missions have provided a wealth of data on the atmospheres and aeronomy of rocky planets and moons, from the lower layers up to the external envelopes in direct contact with the solar wind. This session solicits contributions that investigate processes at work (chemistry, energetics, dynamics, electricity, escape, surface-atmosphere interactions, etc...) in the lower, middle and upper atmosphere of the terrestrial bodies of the Solar System. Contributions based on analysis of recent spacecraft and ground- based observations, comparative planetology studies, numerical modelling and relevant laboratory investigations are particularly welcome. In view of the three future Venus missions selected by ESA and NASA, papers discussing contemporary Venus atmospheric science in preparation for these missions are also encouraged. The session will consist of invited and contributed oral talks as well as posters.

Collisional processes are integral mechanisms that both shape the final configuration of the Solar System, and modify planetary surfaces and small bodies from its birth until today.
This session aims at understanding planetary impact processes at all scales, in terms of impact cratering and ejecta dynamics, crater distribution and crater chronology, material mixing, shock metamorphism and other geochemical consequences, ejecta-atmosphere interactions, impact induced climatic and environmental effects, and biotic responses.

We welcome oral and poster presentations across this broad range of studies about natural or artificial impact collision phenomena on planetary surfaces and small bodies. In particular, abstracts on impact modelling, impact laboratory experiments, geologic and structural mapping, petrographic and geochemical analysis of impact products, as well as remote sensing observations from space missions to planets and small bodies. We also welcome the examination of competing hypotheses for the giant impact formation of terrestrial and outer solar system bodies.

Venus, often referred to as Earth's sibling due to its similar size, mass, and proximity, remains one of the most intriguing and enigmatic planets in our Solar System. Despite these similarities, Venus has followed an evolutionary path that is drastically different, presenting a profound enigma for planetary scientists.
Today, Venus is once again in the spotlight of planetary exploration, with an exciting wave of missions set to transform our understanding of this enigmatic world. Future missions such as ESA's EnVision and NASA's VERITAS and DAVINCI aim to explore Venus, uncovering clues about its geological history and activity, interior structure, atmospheric composition, and climate evolution. Beyond these missions, a diverse array of scientific activities, including ground-based observations, laboratory experiments, and theoretical modeling are contributing to a comprehensive understanding of Venus.
We welcome contributions from all areas of Venus research, including interior processes, surface geology, atmospheric dynamics, laboratory simulations, and mission data analysis. By bringing together diverse expertise, this session aims to enhance our understanding of Venus' history and current state, while exploring its broader implications for planetary evolution throughout the Solar System and beyond.

Volcanism and tectonics are two of the most ubiquitous processes at work in the Solar System, substantially shaping the diverse surfaces of terrestrial planets, moons, and icy satellites. High-resolution orbital data, samples from the lunar surface, and seismic data from the Moon and Mars, have provided important constraints on the evolution of planetary bodies and their tectonic regimes. This gives us a much better understanding of how these worlds evolved, how they are internally structured, and why their surfaces look the way they do. Following the success of InSight on Mars, the selection of e.g., Dragonfly, VERITAS, EnVision, Chang’e 6 and the Farside Seismic Suite promise a wealth of additional observations of Titan, Venus, and the Moon that will contribute to furthering knowledge not only of the extent of volcanic and tectonic activity on these worlds, but also of their seismicity. Small body seismology is also becoming a hot topic, with space agencies considering seismometers for inclusion in future missions to asteroids and comets.

This session invites observational, analytical, theoretical, and analogue fieldwork research into any aspect of planetary endogenic processes. We welcome submissions on comparing landforms and processes on multiple bodies; geochemical and chronological data from planetary material; numerical modeling studies; tectonics and seismicity across the Solar System; theoretical and technical designs for current or future missions; as well as data analysis and insights on the seismicity and interior structures of planets and small bodies.

This session on Mars system in-situ science welcomes new results in all areas of planetary sciences using data from past and present landed missions (such as Curiosity, InSight, Perseverance, Zhurong...), as well as studies preparing for upcoming landed missions (such as ExoMars Rosalind Franklin, Mars Sample Return, MMX...), and any relevant updates on these missions. This session also welcomes studies based on terrestrial analogues, laboratory data and/or numerical
modeling that help to understand processes at past, present or future landing sites.

Ionospheres are a fundamental part of planetary and cometary atmospheres that are formed by solar radiation and are affected by a myriad of different processes, such as space weather activity or neutral atmosphere variations. Moreover, ionospheres play an important role in controlling the dynamics of the system, as they are the link between the neutral atmosphere, exosphere and surrounding plasma environments (e.g. the solar wind for Mars, Venus, Pluto and comets, and the Kronian magnetosphere for Titan). Understanding how each unmagnetized body reacts to all these factors is a key in comparative aeronomy because although a priori all of them have a general similar behaviour, they also have scientifically important differences caused by their different natures.

This session focuses on the ionospheres of Mars, Venus, Pluto, Titan, Jovian moons, comets and any related planetology comparative between them and ionospheres of magnetised bodies. We solicit abstracts concerning remote and in situ data analysis, modelling studies, instrumentation and mission concepts. Abstracts on planetary flybys, such as the BepiColombo, Solar Orbiter and Parker Solar Probe flybys to Venus, are also welcome. Topics may include, but are not limited to, day and night side ionospheric variability, sources and influences of ionization, ion-neutral coupling, current systems, comparative ionospheric studies, and solar wind-ionosphere interactions and responses of the ionized and neutral regimes to transient space weather events. Abstracts on general plasma and escape processes are also welcome.

Understanding surface-exosphere coupling has direct implications for past and current planetary data sets, as well as planning and interpreting future exploration missions. This session explores the physics governing the interactions between surface-bounded exospheres and their planetary surfaces, spanning scales from atomistic processes to global dynamics. We welcome contributions from data analyses, laboratory experiments, and simulations aimed at enhancing or integrating our understanding of these interactions. Topics of interest include the physical chemistry of surface–volatile exchange and key drivers such as the plasma environment, micrometeoroid bombardment, and related processes—including space weathering, irradiation, and volatile implantation. We encourage studies that bridge multiple processes or dimensional scales, with a particular emphasis on the bidirectional coupling between surfaces and exospheres, where surface properties influence exospheric behaviour and exospheric processes, in turn, affect surface evolution. We also invite comparative investigations across different planetary bodies (including the Moon, Mercury, and icy moons) to refine the physical description of exosphere–surface interactions. Ultimately, we aim to foster a comprehensive, multi-scale understanding of the physics shaping these environments. The insights gained from this session could have significant implications for planetary science and exploration.

Key Themes:
• Atomistic Modeling: Utilizing atomistic approaches to provide insights and possible validations for larger-scale processes.
• Parameter Identification: Determining key parameters for surface-bounded exospheres and surface interactions at varying scales will inform further atomistic research and guide observational and laboratory experiments.
• Surface–Exosphere Linkages: Explaining the connections between surface-bounded exospheres and their respective surfaces, including compositional and topographic effects.
• Comparative Investigations: Encouraging comparative studies across different planetary bodies (including icy moons) to enhance our knowledge of underlying processes.

By addressing these key themes, the session explicitly links micro-scale processes to macro-scale dynamics, thereby bridging scales and enriching our integrated understanding of exosphere–surface interactions. We particularly encourage early career scientists to submit an abstract for an oral presentation.

The joint ESA/JAXA mission BepiColombo has successfully completed its 6 swingbys of Mercury and is now on a year-long intermission before orbit insertion in late 2026.
Its swingbys reached unexplored regions in the Hermean environment.
Thanks to previous observations by Mariner 10 and MESSENGER and the benefits of numerical modelling,
our understanding of Mercury's origin, formation, composition, interior structure, surface, exosphere and magnetospheric environment can be improved.

The period until orbit insertion provides a valuable opportunity to synthesize lessons learned from modeling, laboratory experiments, Earth-based observations, and data collected during BepiColombo’s cruise phase, as well as from the Mariner 10 and MESSENGER missions.

This session will host contribution efforts in planetary, geological, exospheric and magnetospheric science.
These contributions are based on available spacecraft observations, Earth-based observations, modelling of interior, surface and planetary environment, as well as theoretical and experimental approaches.
We welcome interdisciplinary contributions that "think outside the box" to propose new approaches for future BepiColombo observations.

This session is particularly timely and relevant as the scientific community prepares for the next phase of the BepiColombo mission.
By bringing together diverse contributions, we aim to build a comprehensive understanding of Mercury that will maximize the scientific return of BepiColombo’s orbital observations.

Planetary cryospheres encompass environments enriched of volatile ices, in the form of deposits, polar caps, glaciers, and permafrost. Cryospheres are found across the entire Solar System at very different heliocentric distances: on Earth, ice plays a crucial role in landscape evolution as a key hydrological resource and acts as a valuable paleoclimatic indicator.
Martian polar caps exhibit analog features to those on Earth, including surface modification and associated landforms, but they also contain CO₂ ice. At mid-latitudes, periglacial landforms—such as polygonal terrains indicate the presence of subsurface ice, while glacier-like features provide evidence of past glacial activity. Moreover, airless bodies such as Mercury and the Moon host icy deposits within the permanently shadowed regions of their polar craters. Further away, beyond the frost line, water ice becomes the dominant compositional endmember. All satellites of Jupiter and Saturn have icy crusts. For some of them (Europa and Enceladus) we have clues for the presence of internal oceans. In addition to water ice, CO₂ and CH₄ also condense into cryosphere at extremely low temperatures. Trans-Neptunian Objects (TNOs), and cometary nuclei are the objects more distant to the Sun and their low temperature and orbital properties allow them to be “time-capsules” because preserve the most primitive material in the Solar System.
Therefore, studying ice on various planetary bodies is crucial for understanding their composition, geological history, climate evolution, and the processes that contributed to the formation of the Solar System.
This session welcomes a broad range of contributions, including geological, geophysical and compositional analyses, mapping products, numerical modeling, and laboratory experiments, as well as research incorporating terrestrial analogs.

The lunar space environment is governed by dynamic coupling between the solar wind/magnetospheric plasma, energetic particles, exosphere, dust, photoelectrons, solid surface, and magnetic anomalies. In recent years, almost all space agencies and many private companies and universities have been active in preparation for lunar exploration. Successful exploration in the coming decade will reveal mysteries of the Moon, but on the other hand, they will significantly alter the lunar environment. Characterizing the pristine state before it is contaminated by human activity is an urgent matter, and we should act immediately.

This session invites oral and poster contributions across this broad area of the lunar environment. Key themes include
- Innovative science: Scientific outcomes using a range of methods, including data analysis, numerical simulation, lab experiments, instrumentation, future missions, and a combination of these.
- Pre-contamination characterization: What is needed to characterize the pristine state that is a critical benchmark for evaluating the impact of human activity.
- Interdisciplinary insights: Revealing mysteries of the coupling between different domains of the Moon and the space environment.

This session aims to gain insight into the complex coupling that shapes the lunar space environment, examine the implications for future lunar science, exploration, and human activities, engage with diverse scientists from various disciplines to share cutting-edge knowledge, and spark new ideas about science.

Shape, gravity field, orbit, tidal deformation, and rotation state are fundamental geodetic parameters of any planetary object. Measurements of these parameters are prerequisites for spacecraft navigation and mapping from orbit as well as modelling of planetary internal structure and evolution. This session welcomes contributions from all aspects of planetary geodesy, including relevant theories, observations, planned measurement concepts as well as modeling efforts in application to planets, satellites, asteroids, and comets.

The session includes results from sample return missions, in particular those achieved by the recent OSIRIS-Rex (NASA), Hayabusa2 , (JAXA), Chang’e 5 (CNSA) and Chang’e 6. The aim is to stimulate the discussion on the perspective of future sample return missions, in terms of science and technological value, specifically in view of NASA’s Mars Sample Return mission.
The session is opened, but not restricted, to the following topics: a) new results from in-orbit observations of sample return missions; b) new laboratory analyses on samples returned from OSIRIS-REx, Hayabusa2, Chang’e 5, Chang’e 6 and past missions (e.g., Luna, Apollo, Stardust, Hayabusa); c) preliminary activities for the Mars Sample Return mission; d) preparation, performed studies and expected results from future sample return missions (e.g., Mars Sample Return, Tianwen2); e) new sample return mission concepts; f) technologies and methods for sample return; g) technologies and concepts for curation facilities; h) technologies and concepts for handling, transportation and analysis of
returned samples in laboratory and between laboratories.

The Martian system presents a unique environment with its two peculiar moons, Phobos and Deimos, whose origins remain a matter of debate, with discussions mostly between a giant collision or the capture of primitive asteroids. This session welcomes presentations that explore all facets of the two Martian moons, from their surface characteristics and internal structures to their interactions with the space environment. Topics of interest include, but are not limited to, geophysical investigations, geo-chemical composition, orbital dynamics, and space-weathering processes.
We particularly encourage presentations on scientific results using data from past and present missions as well as abstract addressing the future exploration of Phobos and Deimos, including mission and instrument concepts and developments, and preparation studies for the upcoming JAXA’s Martian Moon eXploration (MMX) mission.

Atmospheric aerosols and cloud particles are found in every atmosphere of the solar system, as well as, in exoplanets. Depending on their size, shape, chemical composition, latent heat, and distribution, their effect on the radiation budget varies drastically and is difficult to predict. When organic, aerosols also carry a strong prebiotic interest reinforced by the presence of heavy atoms such as nitrogen, oxygen or sulfur.

The aim of the session is to gather presentations on these complex objects for both terrestrial and giant planet atmospheres, including the special cases of Titan’s, Pluto's and Triton's hazy atmospheres. All research aspects from their production and evolution processes, their observation/detection, to their fate and atmospheric impact are welcomed, including laboratory investigations and modeling.

Radar observations can provide detailed information on material properties (e.g., composition, porosity, roughness) for planetary surfaces across the solar system. Crucially, ground-based measurements, such as from the Arecibo Observatory in Puerto Rico and the Goldstone Solar System Radar in California, have provided invaluable astrometric information and size constraints for over 1000 near-Earth objects, which have been used to inform planetary defense. Furthermore, for some NEOs, radar imaging has provided meter-scale details of shape and wavelength-scale roughness and spacecraft radars have provided constraints for small-body interiors (e.g., CONSERT on ROSETTA). Across the solar system, radar measurements have discovered in situ resources, such as buried water ice, and informed landing site selection by facilitating geohazard assessment studies.
For more than 50 years, the Arecibo Observatory planetary radar explored the Solar System from Earth, including determining the rotation rate of Mercury, detecting liquids on Saturn’s moon Titan, and observing tens to hundreds of NEOs yearly, many with sufficient data for detailed analysis of surface morphology and 3-D shape reconstruction. Current radar facilities continue monitoring near-Earth space (e.g., Goldstone), as well as emerging capabilities at Green Bank Observatory and southern hemisphere observing capabilities in Australia. Various radar observing methods have also been used to study Solar System bodies in orbit, including synthetic aperture radar imagers (e.g., the Lunar Reconnaissance Orbiter’s Mini-RF), and sounders (e.g., Mars Reconnaissance Orbiter’s SHARAD). Many more such instruments are en route (e.g., RIME on JUICE and REASON on Clipper for Ganymede and Europa, as well as JuRa for 65803 Didymos) and others are in development (e.g., SRS on EnVision, and VISAR on VERITAS for Venus), as well as planned instruments for small body exploration, including the upcoming close-approach of 99942 Apophis (e.g., RAMSES).
In this session, we invite contributions relating to ground- and space-based planetary radars, from the analysis of existing missions and facilities, laboratory and field-analog studies, to instrument development, and new techniques to conduct radar studies.