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.

The characterization of cometary nuclei and their dust, gas and plasma environment is being done through in-situ and remote observations techniques.
In the context of the Rosetta mission and missions to small bodies including Comet Interceptor, and international observing campaigns of bright comets such as 12P/Pons-Brooks, C/2023 A3 (Tsuchinshan-ATLAS), C/2024 G3 (ATLAS), we solicit presentations on recent investigations.

The session will present results of optical, infrared or radio observations of comets and
active bodies obtained from ground-based telescopes, space observatories such as JWST, as
well as recent results from in-situ measurements from space missions.

Interstellar objects (ISOs) have become a novel field of Galactic small body studies, connecting the formation history of our Solar System to the processes of planetesimal creation and evolution that play out in planetary systems across the Milky Way.

The known population of ISOs is expected to increase soon, following 1I/`Oumuamua in 2017 and 2I/Borisov in 2019, as the planetary science community reaps the benefits of a new generation of survey telescopes. At the given epoch, the intrinsic ISO population remains observationally unconstrained; theoretical predictions are equally influential as observed physical characteristics on our understanding.

This session explores the past, present, and future research on interstellar objects, and is therefore open to contributions from a wide range of topics, including (but not limited to):
- Planetesimal formation and ejection mechanisms
- ISO dynamics in the Galaxy
- Evolutionary processing of small bodies e.g. in the interstellar medium or tidal disruption
- The relationships of Solar System populations to ISOs
- Observational characterisation of the known ISO population, 1I and 2I
- Population modelling & predictions for future ISO discoveries
- Mission concepts for in-situ ISO observation

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.

Artificial intelligence (AI) refers to the development of computer software capable of performing tasks that would typically require human intelligence. Machine learning (ML) is a branch of computer science that explores algorithms that can learn from data. ML is primarily divided into supervised and unsupervised learning. In the former, the algorithm is presented with examples of labeled examples, and a training routine is executed to learn a general rule that maps inputs to outputs. In the latter, no label is provided to the learning algorithm, which enables the network to autonomously identify latent and representative structures in the data. Deep learning is a branch of machine learning based on multiple layers of artificial neural networks, which are computing systems inspired by the biological neural networks found in animal brains. This session aims to provide a forum for discussing recent advancements in the applications of AI and ML to planetary science.

The integration of specialized techniques and methodologies from diverse disciplines has become increasingly common in planetary science research in recent years, paralleling the global trend of cross-disciplinary collaboration across scientific fields. Recent high-profile recognitions of interdisciplinary research contributions (e.g. Nobel Prize in Physics and Chemistry) have further fueled the utilization of external expertise across all subfields of planetary science.

Current publications on cross-disciplinary adaptations typically follow two approaches: principal investigators acquiring the necessary expertise themselves, or establishing partnerships with specialists from other fields to supplement the required knowledge. However, engaging with rapidly evolving disciplines, where innovations emerge frequently, presents significant overhead for interdisciplinary researchers. This cross-disciplinary trend is expected to intensify with the growing complexity of planetary science questions.

This session aims to explore various forms of engagement between planetary scientists and experts from other disciplines such as data science, chemistry, biology, geology, engineering, physics, social sciences, and other complementary domains. We invite contributions addressing:
- Knowledge transfer strategies across discipline boundaries
- Resource allocation and management in interdisciplinary projects
- Communication protocols and best practices for bridging disciplinary terminology gaps
- Lessons learned from both successful and challenging experiences
- Initiatives facilitating cross-disciplinary engagement

Astrobiology is the study of whether present or past life exists elsewhere in the universe. 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.

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 years, new astronomical instruments 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 physical and technological horizon will allow us to overcome the 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 environment 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.

Unlike the Hertzsprung–Russell diagram for stars, there remains as yet no formal classification for solid exoplanets composed of varying proportions of fluids, rock+metals and ice. Still, as with stars, planetary mass and composition – expressed in geochemical and cosmochemical terms – modulate bulk physical and chemical characteristics that may be detectable by remote observations of exoplanet atmospheres. How can the physical and chemical attributes that control rocky exoplanet interiors (exo-geodynamics) be determined via theory, simulation, observations, phenomenology and experiments? Specific examples include: using galactic chemical evolution to relate the properties and compositions of host stars and their exoplanets; relating chemical geodynamics of rocky planet interiors to system age, stellar class, luminosity and XUV evolution; and, how these properties manifest themselves observationally in the spectra of exoplanetary atmospheres. We invite contributions in the broad new area of geoastronomy that unify principles from astrophysics and the geosciences to advance our understanding of rocky exoplanets in the JWST era and beyond.

This session seeks papers on the biological, physicochemical, astrophysical, and paleontological studies of the living-matter origination problem, conditions necessary and sufficient for living-matter origination and development, mechanisms of living-matter origination on the Earth and other celestial objects, 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 welcomed.
This includes work related to theme of the Origins of Life to study interstellar chemistry, meteorites and comets chemistry as well as the chemistry of planets.

With JWST scientifically operational since mid-2022, and PLATO and ARIEL on the horizon, we are now in the middle of a decade of exoplanet characterization. We therefore invite abstracts to this session with a focus on the characterization of rocky to sub-Neptune. This includes modeling of their internal chemical composition and structure, density and age, laboratory experiments and ab initio calculations, thermal evolution models, and atmospheric evolution models. We also invite abstracts focussing on the observational capability of current and upcoming space missions and ground-based telescopes to characterize low-mass to Neptune-size exoplanets. Our aim with this session is to foster the discussion between modelers, experimentalists and observers especially in preparation for the PLATO and ARIEL space missions.

Solar system analogs host a remnant of the protoplanetary disks around the central star, the so-called debris disks. These are formed as a by-product of planet formation and consist of material left over from planet formation, such as dust, gas, and planetesimals belts. Due to dust's short lifespan, it requires continuous replenishment through planetesimal collisions, highlighting the interconnected nature of these components. Additionally, substellar companions can significantly influence dust and planetesimal dynamics through gravitational effects. Even Earth-sized planets can leave distinctive marks on debris disk structures, while misaligned planets or those with elliptical orbits may reveal past gravitational interactions. Thus, tracing substellar companions such as planets or perturbers within debris disks can provide crucial insights and constraints into their evolution.
Using N-body simulations, SPH simulations, and collisional evolution models of debris disk systems, the community demonstrated observable planet-disk configurations with large-scale signatures of the brightness distributions (e.g., spiral structures and/or two local azimuthal maxima). These features are potentially detectable using high-resolution near-to-mid infrared imaging facilities.
In this session, we will discuss recent observations of possible planet-disk interactions using JWST and VLT/ERIS, placing them in the context of debris disk simulations that incorporate planetary interaction. We will also highlight how future instruments on the ELT, such as MORFEO/MICADO or PCS, will enhance our understanding of the formation, architecture, and evolution of planetary systems in solar system analogs.

The coming years will be revolutionary for rocky planet research, with JWST, ELT, ARIEL, and PLATO providing unprecedented observations of rocky exoplanets in our galaxy. At the same time, BepiColombo, the Mars sample return mission, and the Decade of Venus missions will greatly enhance our understanding of the rocky bodies within the Solar System. These missions will offer valuable new observations of the atmospheres and surfaces of these rocky bodies, while Solar System missions will also probe magnetic fields. Interpreting these observations, and leveraging them to constrain the body’s interior properties, requires a deeper understanding of how a planet’s surface, atmosphere, and interior interact.

Rocky planet atmospheres and surfaces form and evolve under close interaction with their deeper interiors. Whether a planet has formed an atmosphere by volatile exchange with a magma ocean, by volcanic outgassing, or lost its atmosphere completely, understanding its observed state requires knowledge of interconnected processes operating across a wide range of spatial and temporal scales. Processes governing atmospheric evolution, and how it interacts with the interior, include volcanism, weathering, tectonics, magnetic field generation, interior and atmospheric volatile chemistry, and atmospheric loss. These processes operate on various timescales, from rapid magma-atmosphere equilibration, to the shaping of tectonics on the early Earth, to long-term climate feedbacks that sustain temperate conditions on planets like Earth. Studying these interactions - both in the Solar System and beyond - demands a fundamentally multidisciplinary understanding of rocky planets, spanning astronomy, geosciences, and planetary sciences.

This session aims to bring together scientists from astronomy, geosciences, and planetary sciences, to explore how interior-atmosphere interaction shapes rocky (exo)planet surfaces and atmospheres. We welcome contributions spanning experimental work, observational efforts, and modelling studies. By combining insights from exoplanets, which serve as a natural laboratory for rocky world diversity, and Solar System planets, which provide the detailed observations needed to build and validate models, we can develop a robust framework for interpreting observations of any rocky body. We encourage discussions that span all related fields, fostering new collaborative approaches to studying rocky planet evolution.

A quarter century after the first exoplanet transit was observed, there are now over 4000 known transiting exoplanets. Many planets now have 100-1000+ transit light curves stretching spanning 3+ decades thanks to prediscoveries. This historical record provides a valuable resource to search for temporal changes over both short and long timescales, leading to many subfields of exoplanetary research including: finding small companion planets using transit timing variations; identifying changing orbital periods due to orbital decay, precession, or other effects; searching for seasonal atmospheric changes; tracking starspot crossings; or searching for exomoons.

All of these endeavors, however, require precise transit record-keeping for reliable results, since they must combine results from many instruments and research groups. However, the steady stream of new data combined with the lack of any authoritative archive makes it difficult even to compile a complete and accurate list of past observations. Worse, errors that have crept into the scientific literature are hard to eliminate, since they may pass through multiple published works before being identified. It is also often not possible to return to the original data since many papers continue to be published without making public transit light curve data, sometimes without even providing individual transit midtimes.

This session aims to bring the community together to discuss problems relating to long-term transit studies. Relevant session topics include: (1) the challenges of precise and accurate timing, including best practices for small and citizen science telescopic observations; (2) recommendations for best publication and citation practices, including transit light curve archiving and proper identification and tracking of prior observations; and (3) any research topics in long-term transit studies that would benefit from improved archival practices. We also welcome presentations on long-term studies of planetary occultations (or secondary eclipses), which are subject to the same archival issues and are even less likely to have publicly available source data.

This session is co-organized by both the Exoplanet Transit Database and the Short Period Period Group, or SuPerPiG, which is leading a NASA-funded pilot effort to investigate, compile, and archive lightcurves from the transit literature.

James Webb Space Telescope observations are tentatively revealing a pattern of airless or thinly blanketed worlds around low-mass stars, evidenced in part by a lack of “dayside cooling.” This raises a fundamental question—following the escape of primordial hydrogen, when will ionising irradiation also evaporate the high-molecular-weight atmospheres supplied by volcanism on a rocky planet? The 500-hour Rocky Worlds DDT program will probe this question, guided by the hypothesis that atmospheric escape sculpts a Cosmic Shoreline. However, before the puzzle can take shape, its pivotal pieces require further exploration and debate:
* What are the strongest atmospheric constraints we can infer from transmission and emission observations?
* What are the optimal observing strategies to detect atmospheric features?
* Under what conditions can a bare rock revive an atmosphere?
* How well do we understand M-dwarf evolution, particularly X-ray flare activity over time?
* What level of ionising irradiation can drive hydrodynamic escape of metal-rich atmospheres, and how does this process depend on planetary mass?
* How will the launch of ELT, PLATO and ARIEL boost atmospheric characterisation?
We invite contributions that explore observations (both real and simulated) and models of star-planet evolution (including interior, atmospheric, and escape processes). If some of the rocky planets in the habitable zones of the galaxy’s most common stars can retain their atmospheres, the universe could be teeming with life—and astronomers just might be able to observe its signatures in the near future.

The past few years have witnessed major developments in the field of terrestrial planet formation. Thanks to the advances in computational technology, the three leading scenarios, namely, the traditional model, pebble accretion, and formation in rings, have become more complex, and have demonstrated their broad and expansive success. How these three approaches compare, and how they contribute to developing a comprehensive model of terrestrial planet formation are now among the most outstanding questions in planetary astrophysics. Through a collection of invited talks and contributed oral and poster presentations, this session aims at introducing each approach and assessing their capabilities by comparing their results to our knowledge of terrestrial planets in our solar system and extrasolar planets. As part of this session, we also plan to organize a press conference or town hall, where renowned experts from each formation scenario will answer questions from the press and an audience of peers.

We cordially invite all experts and interested colleagues to submit abstracts for oral and poster contributions in all areas related to theoretical, observational, and experimental studies of terrestrial planet formation in our solar system and extrasolar planets. We strongly encourage contributions from early career scientists.

The number of known planetary systems continuously grows, revealing an increasingly complex nature of extrasolar worlds, challenging our understanding of planetary system formation and evolution.

In this session, we address the question of the intricate dynamical evolution of RV-detected systems and transit-detected planetary systems, where resonant and chaotic processes emerge from complex gravitational interactions. Additional effects, including tidal forces, general relativistic effects, planet-disc interactions, and the gravitational influence of binary companions, can strongly affect the architecture and long-term stability of such systems.

This session aims to explore how theoretical modeling can provide crucial insights into system characterization by confronting dynamical predictions with observational constraints, highlighting how dynamical constraints inform our interpretation of planetary system architectures from initial formation to long-term evolutionary states.

JWST has enabled researchers across the globe to probe the atmospheric composition of exoplanets and investigate the properties of distant planetary systems. Future confirmed and conceptual campaigns such as the ELT, HWO and LIFE aim to pay greater attention to Earth-mass planets orbiting within the habitable zones of their host stars. In anticipation of these missions, this session focuses on the current and future search for biosignatures within the atmospheres of exoplanets, the identification of habitable worlds and the exploration of planetary conditions that support habitability. It solicits contributions from both observers using data collected by past and present instrumentation, as well as atmospheric, stellar activity, and interior modellers looking towards future observations. The session aims to foster new collaborations with observers, modellers, and instrument team members to assess how markers of life and habitability in distant systems may present themselves to us, and the requirements that future observing campaigns need to reliably identify them within planetary parameter space.

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.