The orbital stability of (exo-)planetary systems is far from trivial, as chaotic diffusion can strongly affect the long-term evolution of planetary orbits. Mean‑motion and secular resonances may act as stabilizing mechanisms, constraining the range of orbital parameters compatible with current observations. A variety of additional dynamical processes further shape system architectures, including perturbations on close‑in exoplanets, resonant interactions involving giant planets, planetesimal scattering during and after formation, and episodes of planetary ejection driven by collisions or tidal disruptions.

This session aims to bring together observational, theoretical, and modeling studies that investigate the dynamical pathways of these systems, from early formation stages to mature planetary systems, and to understand how these mechanisms interplay for interpreting observed architectures and assessing the long‑term stability of both compact and widely separated planetary systems.
We welcome contributions employing numerical simulations, N-body studies, stability analyses and observational constraints.

Artificial intelligence (AI) is revolutionizing planetary sciences, enabling new insights from vast and complex datasets, both for solar system exploration and the study of exoplanets and brown dwarfs.

This session will explore AI-driven approaches for studies, focusing on innovative techniques such as image analysis, curriculum learning, diffusion models, generative models for data augmentation and simulation, machine learning techniques for analyzing large-scale surveys. We will also discuss applications of natural language processing for scientific literature mining, and uncertainty quantification in AI-driven models. By bringing together experts in AI and exoplanetary science, this session aims to foster interdisciplinary collaborations and advance the field.

Exoplanets are being discovered in large numbers thanks to recent and ongoing surveys using state-of-the-art instrumentation from the ground and space. In the next few years, new astronomical instruments (such as Nancy Grace Roman, PLATO, CHORUS, SAXO+, ANDES, Ariel, ELF, HWO and others) will scout ever more distant regions of our Galaxy, and they will validate new technology for the ultimate direct characterisation of temperate exoplanets. Such a change in the physical and technological horizons will allow us to overcome current observational biases in the search for alien worlds and to gain a deeper understanding of the chemical and physical properties of exoplanets and the environments that surround them. Ultimately, we will be able to unveil processes of formation and evolution of planets, together with those of their atmospheres, on a scale much larger than our Solar Neighbourhood.

The goal of this session is to bring together the instrumentation and observational communities that are underpinning the future of this field. Contributors are invited to review ongoing programmes of discovery and characterisation of both exoplanet and circumstellar discs, to update on the progress of planned instrumentation programmes, and to present innovative ideas for future instrumentation.

Astrobiology is the study of whether present or past life exists elsewhere in the universe. Planetary Habitability refers to the conditions of a planetary body to be habitable. To understand how life can begin in space, it is essential to know what organic compounds were likely available, and how they interacted with the planetary environment. This session seeks papers that offer existing/novel theoretical models or computational works that address the chemical and environmental conditions relevant to astrobiology on terrestrial planets/moons or ocean worlds, along with other theoretical, experimental, and observational works related to the emergence and development of Life in the Universe. This includes work related to prebiotic chemistry, the chemistry of early life, the biogeochemistry of life’s interaction with its environment, chemistry associated with biosignatures and their false positives, and chemistry pertinent to conditions that could possibly harbor life (e.g. Titan, Enceladus, Europa, TRAPPIST-1, habitable exoplanets, etc.).
Understanding how the planetary environment has influenced the evolution of life and how biological processes have changed the environment is an essential part of any study of the origin and search for signs of life. A central issue in the research on the emergence of life is the paradoxical role of water in pre-biotic chemistry. In fact,on the one hand, water is essential for all known life, on the other hand it is highly destructive for key biomolecules such as nucleic and polypeptides. Earth analogues experiments/instruments test and/or simulation campaigns and limits of life studies are included as well as one of the main topics of this session.

Major Space Agencies identified planetary habitability and the search for evidence of life as a key component of their scientific missions in the next two decades. The development of instrumentation and technology to support the search for complex organic molecules/sings of life/biosignatures and the endurance of life in space environments is critical to define unambiguous approaches to life detection over a broad range of planetary environments. A truly interdisciplinary approach is needed to delve into the core of the issue of emergence of life, because in addition to physics and chemistry it is also need to deploy a number of other sciences. We rely on contribution coming from mathematical or philosophical perspectives not only on astrobiology moreover we think that a part of the answers may lie in scientists who working on cancer research, genetics, space exploration paleontology who are not necessarily involved in this field.

The properties of exoplanets are closely linked to their formation environments and to the physical and chemical characteristics of their host stars. Over the past decade, significant advances in high-precision stellar characterisation, resolved observations of protoplanetary disks, and extensive exoplanet surveys have substantially improved our understanding of how planetary systems emerge and evolve. Detailed stellar abundance measurements now provide key constraints on disk composition and initial conditions for planet formation. In contrast, observations of disk substructure and chemistry reveal the processes that regulate accretion, migration, and mass loss. At the same time, statistical studies of exoplanet demographics have uncovered correlations between host star properties, planetary architectures, and atmospheric characteristics, highlighting the importance of a unified star–disk–planet framework. This session aims to bring together observational, theoretical, and modelling studies that investigate the physical and chemical pathways linking stars, disks, and planets, from early formation stages to mature planetary systems, and to assess how these connections shape the diversity of exoplanetary atmospheres and system architectures observed today.

Exploration of the solar system and astrophysics missions have revealed remarkable insights into the composition, chemistry, and biological potential of the giant planets, their moons and ring systems, smaller bodies beyond Neptune, the interstellar medium, and protoplanetary disks. Many of these bodies have become key targets for understanding the origins of life on Earth and other celestial objects. Increasingly sophisticated ground- and space-based instrumentation enables new observations and in situ measurements of these fascinating environments, which will facilitate novel chemical and biological investigations at the forefront of planetary science.

Carbon chemistry is ubiquitous in the dense interstellar medium, with chemical modelling, laboratory experiments, and astrophysical observations suggesting that the complex macro-molecular building blocks of life could be synthesised in ices under these conditions. Such material can be incorporated into planetesimals during their accretion, and planetary bodies can today play host to complex chemistry. This is significant across many aspects of exploration in the outer solar system, particularly in the potentially habitable satellites of the giant planets. The subsurface liquid water oceans of the moons Enceladus (the only extraterrestrial ocean to have been sampled) and Europa are likely habitable, whilst Titan could be a natural prebiotic laboratory. Clearly, the characterisation of these fascinating geochemical environments is critical to understand habitability and search for extraterrestrial life. The New Horizons mission and JWST observations have characterised the compositions of primitive Trans-Neptunian Object (TNOs) in the farthest reaches of the solar system, enabling a direct comparison with the ices in protoplanetary disks that are the feedstock for carbonaceous molecules in extra-solar planetary systems.

This symposium will discuss our current understanding of chemistry and the emergence of life in the solar system and beyond, welcoming contributions related to icy ocean worlds, ring systems, comets, asteroids, surfaces, TNOs, protoplanetary disks, and the interstellar medium. Results derived from space mission data, detections of organic molecules via telescopic observations, laboratory experiments predicting or characterising chemical processes, and theoretical approaches including quantum chemistry and geochemical modelling are encouraged. We encourage submissions on biological, physicochemical, astrophysical, and paleontological studies of the living-matter origination problem, the conditions necessary and sufficient for living-matter origination and development, mechanisms of living-matter origination on the Earth and other celestial objects. Submissions on promising celestial objects for the living-matter occurrence, and other experimental, theoretical, and observational works related to the emergence and development of life in our Solar System and beyond are also welcomed.

This session aims at establishing a regular and accessible meeting opportunity across Europe for the international SETI (Search for Extraterrestrial Intelligence) community. It encourages participation from various fields of research, facilitating collaboration among these fields and SETI, with the objective of helping establish an interdisciplinary and collaborative SETI community.
The Search for Extraterrestrial Intelligence is an expanding field, crossing several research topics, including:
--Search for radio, infrared, and optical signals emitted by an intelligent civilization (techno-signatures) or large-scale technological development in the Milky Way and beyond; Engineering and space research;
-- Astrobiology, and the potential for life outside our own solar system;
--Outreach and communication of SETI and astrobiology research, its history, achievements, and present and future objectives;
--SETI and citizen science;
--Artistic practices and research in SETI, including science fiction and film making;
--SETI and cognitive sciences, including AI applications in techno-signature search;
--Comparative studies in animal cognition.

The mechanisms of formation, evolution, and migration of giant and rocky planets remain
unconstrained despite the huge progress of the field since the discovery of the first planets in 1995. Understanding planet formation processes is key to improve our knowledge on the origin of planetary systems and our Solar System. The study of exoplanets at young ages (below the age of the Hyades ~600 Myr) is fundamental to determine the timescale of the formation of planets and constrain the dynamical models of planet evolution.

Many exoplanets orbiting young stars have been reported over the past few years in young stellar forming regions, open clusters and moving groups have well-constrained ages and well-determined physical properties (mass, radius, density, temperature), essential to refine evolutionary models based on orbital migration or photo-evaporation. The availability of space-borne missions (Kepler, TESS, Gaia, JWST), high-resolution and high-precision spectrographs (e.g. HARPS, CARMENES, ESPRESSO, SPIRou, etc...), and (sub)-millimetre facilities (e.g. JCMT, SMA, ALMA) have revolutionised the field over the past years.

The goals of this session are to offer a review on the observational techniques and theoretical modelling efforts in the field of young exoplanets, highlight the latest discoveries, and propose a way forward to gain a better understanding of how planetary systems form and evolve. We will divide the session with dedicated contributions on direct imaging, radial velocity, transit timing variation, and transit spectroscopy as well as computer modelling.

The origin of the molecular universe, comprising hundreds of species detected by astronomical observations and space missions, is a central question linking astrochemistry with (exo)planetary science and astrobiology. James Webb Space Telescope (JWST) now directly probes interstellar and disk ices at unprecedented sensitivity, revealing that interstellar icy mantles are already rich in H₂O, CO₂, CO, CH₄, NH₃, and even complex organic molecules (COMs). Strikingly, many of these species share chemical similarities with volatiles observed in cometary bodies, suggesting chemical continuity from molecular clouds to planet-forming environments.

Interstellar ices are not merely passive reservoirs; they act as molecular factories where simple species are transformed into increasing chemical complexity through surface reactions, UV-driven photochemistry, and thermal processing. These icy mantles store and transport volatile material that ultimately becomes incorporated into protoplanetary disks and nascent planets. Understanding how molecules form, evolve, and survive in the solid state is therefore essential for tracing the chemical inheritance of icy bodies in planetary systems.

This session places solid-state chemistry at the center of the molecular inheritance problem, examining how icy grain mantles regulate the chemical inventory ultimately incorporated into forming planetary systems. Key topics include gas–grain chemistry, reaction networks and rates, energetic and thermal processing of ices, volatile transport and reprocessing in disks, and the transmissive and reflective spectroscopic characterization of molecular solids at high resolution. We invite contributions spanning laboratory astrochemistry of ices and organics, chemical modeling, and JWST ice observations in molecular clouds, (proto)planetary systems, icy moons, and comets to develop physico-chemical frameworks that unify chemical networks and constrain the volatile inventories inherited by forming planets.

Recent results from Juno and Cassini have transformed our view of Jupiter and Saturn, revealing complex interior structures, non-uniform mixing, and deep processes coupled to atmospheric circulation and long-term evolution. In parallel, JWST and ground-based observatories are delivering unprecedented data of both Solar System giants and exoplanets, enabling direct comparisons of chemistry, thermal structure, clouds/hazes, and atmospheric dynamics across a wide range of irradiation and ages. Together, these advances create a timely opportunity for comparative planetology that bridges Solar System and exoplanet communities and connects observations with physical understanding.
This session welcomes contributions on giant planets in the Solar System and beyond, with a broad scope spanning observations, lab experiments and theory. Topics include (but are not limited to): formation, evolution, and interior structure, interior-atmosphere connections, atmospheric composition and chemistry, clouds and hazes, circulation, jets and atmospheric variability, and comparative analyses connecting Solar System gas giants, ice giants, and exoplanet populations. We also welcome studies using JWST and ground-based facilities, as well as work that combines multi-wavelength datasets, experiments and modelling to interpret emerging observations.
The session aims to strengthen the physical links between Solar System giants and exoplanet populations through comparative studies grounded in both data and theory.

The first steps of planet formation occur when the young protostar (less than half a million years old) is still heavily accreting material, the planet-forming disk is growing, and the system itself is still enshrouded in the dust and gas of the natal cloud. Due to recent advances in observational studies with ALMA, JWST, and VLT, as well as theoretical work on the earliest stages of protostellar evolution, a wealth of information on those ‘first days’ of planets has been uncovered.
This session aims to present recent advances in protostellar studies and their impact on planet formation, Solar System studies, and exoplanet characterization, with the goal of strengthening links among those communities and experts in protostellar studies. The session invites contributions from theoretical and observational studies of young protostellar systems, including, but not limited to:
- Molecular and elemental composition of young disks and their comparison to mature ones
- Dust in the young disks and of the protostellar system: thermal processing of interstellar solids and minerals condensation, radial dust transport and refractory content of the jets, first stages of grain growth
- Infall and accretion onto the youngest protostars and their impact on the disk evolution, tracers of ongoing planet formation and accretion onto protoplanets
- Comparison of protostellar data with Solar System record of condensation of solids, the formation of chondrules, and the accretion of planetesimals.

This session will focus on the latest research concerning the most numerous class of exoplanets: small worlds, encompassing rocky planets like Earths and Super-Earths, as well as volatile-rich planets like Mini-Neptunes. We invite contributions that explore the properties, formation pathways, and habitability potential of these key planetary types.

The session also includes contributions that explore the evolution of rocky exoplanets from the perspective of changes to the composition of the Galaxy with time. For example, the inventories of the principal long-lived heat-producing elements, HPEs, 40-K, 235-238-U and 232-Th, are encoded in stellar metallicity, age, and nucleosynthetic history. Yet, the long-term thermal evolution of rocky exoplanets driven by different HPE inventories is often overlooked, even though this evolution is a critical factor in interpreting physical properties including retrieved data for secondary and hybrid atmospheres.

Key areas of interest include:

Atmospheric Characterization: New results on the composition, structure, and dynamics of the atmospheres of small exoplanets, utilizing facilities like JWST and focusing on the volatile content, clouds, and potential detection of biosignatures. This also includes work on secondary and hybrid atmosphere generation.

Mass-Radius Relationship and Interior Structure: Studies that probe the transition between rocky Earths/Super-Earths and volatile-dominated Mini-Neptunes, including interior modeling, precise density measurements, and the physical processes driving atmospheric loss, e.g., photoevaporation.

Formation and Evolution: Theoretical and observational work investigating the birth environments, migration, and long-term evolution of small planets, particularly concerning their initial volatile budget and the influence of the host star. This also includes the long-term thermal evolution of rocky exoplanets driven by different HPE inventories and the expression of different evolutionary tracks as a function of parameters such as system age.

Detection and Demographics: Advances in the discovery and precise characterization of small exoplanets from current and future surveys, e.g., TESS and PLATO, and studies of their occurrence rates and population demographics across different stellar types.

Galactic Chemical Evolution and Rocky Exoplanets: Contributions that report current understanding of how galactic chemical evolution, GCE, processes affect the abundances of the rock-forming elements, Mg, Si, O, Al, Fe, Ca, Na, K, on controls for the abundances of HPEs, and on plausible radiogenic heat budgets of rocky exoplanets across different stellar populations in the Milky Way.

The session encompasses work related to observational, theoretical and experimental studies of small exoplanets, including rocky exoplanets connecting GCE and nucleosynthesis with exoplanetary geodynamics, as well as how these affect magnetic dynamo generation, volcanic activity, and secondary/hybrid atmosphere generation.

The session aims to advance our understanding of the fundamental physics governing the formation and diversity of the most common planets in the Galaxy and their potential for hosting life.

The asteroids in particular and the asteroid-comet-dwarf planet continuum in general bear the signature of the birth of the solar system. Their observed properties allow for testing theories regarding the evolution of the solar system's planetary objects and of their prospective development. Additional important insights into this exciting field of research are provided by the laboratory investigations of the samples delivered to the Earth in the form of meteorites and by sophisticated numerical models.
The session will gather researchers of different communities for a better understanding of the evolution and properties of small bodies, ranging from planetesimals or cometesimals to icy moons, and including meteorite parent bodies. It will address recent progresses made on physical and chemical properties of these objects, their interrelations and their evolutionary paths by observational, experimental, and theoretical approaches.
We welcome contributions on the studies of the processes on and the evolution of specific parent bodies of meteorites, investigations across the continuum of small bodies, including comets and icy moons, ranging from local and short-term to global and long-term processes, studies of the surface dynamics on small bodies, studies of exogenous and endogenous driving forces of the processes involved, as well as statistical and numerical impact models for small bodies observed closely within recent space missions (e.g., AIDA, Hayabusa2#, Lucy, New Horizons, OSIRIS-APEX).

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 observational & laboratory investigations and theoretical modelling.

Observations of Interstellar Objects (ISOs) passing through the solar system allow for the direct examination of planetesimals from other star systems. The passage of the third known interstellar object (ISO), 3I/ATLAS, through the solar system has produced the largest set of spacecraft observations for any comet or ISO to date, with observations were obtained from a total of 24 spacecraft to date, including interplanetary spacecraft, a number of solar probes, and 6 astronomical space telescopes. This session invites presentations on science results from terrestrial and spacecraft observations of all three known ISOs, on how the lessons learned from their observation can be applied to future interstellar targets of opportunity, and on plans for future ISO interceptor missions.

Carbon-bearing matter with a wide range in molecular size and structure is found throughout our Solar System. It ranges from simple molecules like CO2 in Venus’ atmosphere to complex mixtures of carbonaceous phases found in Titan or on the Martian surface. The widespread nature and diversity of carbon-based molecules leaves us wondering: How did they form and how do environmental processes transform them? Did this chemical complexity emerge in the Solar System or is it inherited from pre-Solar stages – or perhaps a combination of both? Can organic molecules be used to decipher physical conditions, chemical transformations, and formation histories of planetary bodies and of the Solar System itself? How does the inventory of organic matter influence the emergence and evolution of habitable worlds?

Addressing these complex questions requires a multifaceted and collaborative approach. We therefore invite scientists from all backgrounds and disciplines studying carbon chemistry and its evolution, from primitive bodies to rocky planets and habitable worlds. Whether extracting organic molecules from meteorites, observing KBOs with JWST, analyzing the composition of Ceres as measured by Dawn or future missions, investigating ancient Martian lakes with rovers, simulating hydrothermal processes in asteroid parent bodies, or modeling the Venusian clouds … — all are welcome to contribute to this session to help understand the role and fate of carbon-based matter and to pave the way for future space exploration missions.

Understanding why planetary atmospheres look the way they do today - and reconstructing the evolutionary pathways that brought them to their present states - is one of the most compelling questions in modern planetary science. This session adopts a comparative planetology perspective, bridging solar system bodies and exoplanet populations through the lens of atmospheric evolution, investigated through observations, modelling, and mission-driven science.
Space missions have delivered a wealth of observations of the atmospheres and aeronomy of rocky planets and moons, from the lower atmosphere to regions interacting directly with the solar wind. With recent advances and forthcoming missions, planetary atmospheric science is entering a particularly active phase. This session invites contributions on the physical and chemical processes shaping the lower, middle, and upper atmospheres of terrestrial bodies in the Solar System and beyond, including atmospheric chemistry, energetics, dynamics, electrodynamics, atmospheric escape, surface–atmosphere interactions, and coupling with the space environment. We welcome studies based on spacecrafts (e.g., Messenger, BepiColombo, Venus Express, Akatsuki, EnVision, Davinci, Mars Express, MRO, TGO, EMM, MAVEN, MMX, among others), ground-based observations, numerical modelling, and laboratory experiments.
We welcome contributions addressing the long-term evolution of atmospheres across all planetary types. In the inner solar system, Venus and Mars stand as striking cases of evolutionary divergence from Earth. In view of upcoming ESA and NASA Venus missions, contributions addressing current understanding, open questions, and preparatory studies of the Venus atmosphere and its long-term history are particularly encouraged, from photochemistry and cloud dynamics to the transformative science expected from ESA's EnVision (and its VenSpec suite) and DAVINCI.
In the outer solar system, Titan's organic-rich and seasonally evolving atmosphere offers a unique window into photochemical complexity and long-term change, with new observational and modelling efforts building on the Cassini legacy. The gas and ice giants - characterized with unprecedented detail by JWST, Juno, and the forthcoming JUICE mission - further enrich this comparative picture; ice giant atmospheres in particular represent a frontier for solar system science and an archetype for the most abundant planetary class in the galaxy, with the scientific case for a Uranus mission gaining momentum under NASA's Decadal Survey and ESA's Voyage 2050 framework.
Finally, broader comparative studies linking solar system atmospheric structure and chemistry to the growing population of exoplanets accessible to spectroscopic characterization are warmly welcomed. This includes contributions on atmospheric escape and its demographic imprints on exoplanet populations - from the radius valley and the Neptune desert to observations of young systems caught in the act of losing their envelopes. Both observational and modelling contributions are welcome, as well as cross-disciplinary studies connecting solar system and exoplanet atmospheric science through laboratory measurements, modeling and/or observations.
The session will include solicited and contributed oral presentations, as well as posters.

Since the Galileo mission found evidence for global subsurface oceans at Jupiter’s icy moons over 30 years ago, the icy moons of the giant planets have become central targets of planetary science and astrobiology. The Cassini discovery in 2005 of plumes sourced from Enceladus’ global ocean further raised the interest. Now, with the highly anticipated arrival of NASA’s Europa Clipper & ESA’s Juice spacecraft in the Jovian system in the early 2030s, and NASA’s Dragonfly planned for launch in 2028, there is a growing buzz of excitement about what these missions could uncover.

At the same time, the selection of Enceladus as the primary target of ESA’s L4 mission highlights the importance of preparing for the long-term future of ocean world exploration today. With a landing tentatively on the timeline for the 2050s, this mission has the potential to revolutionise our understanding of the ocean chemistry, habitability, and astrobiology of these worlds.

This session will explore the common physical and chemical processes within the diverse population of the ocean worlds of our solar system. We welcome a broad range of abstracts covering:

Transport of material from ocean to surface and how this may lead to mission observables
Geophysics comparisons between bodies
Aqueous and prebiotic geochemistry
Lab experiments aimed at characterising their interiors or surfaces.
Surface phenomena including geophysics, impacts and space weathering
Constraints on conductive heat flow, ocean composition, and other global properties utilising existing observations and/or modelling

With the advent of Juice, Europa Clipper, Dragonfly, and the progressing planning for ESA L4, we particularly look forward to accepting abstracts relating to to these mission targets, as well as studies of other candidate ocean worlds such as Callisto & Triton, and current efforts aimed at maximising the scientific return of these missions.