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.

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 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.

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.

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.