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. Finally, we also support abstracts investigating the DART impact, whose outcome will be observed by HERA few months after this conference.

This session focuses on the connections between various types of small bodies in the Solar System, including comets, asteroids, and centaurs, while emphasising their activity at different distances from the Sun. Special attention will be given to analysing the activity of small bodies in the context of their evolution, as well as addressing open questions and unresolved issues in this field. The session will also highlight the importance of monitoring and archival data, which serve as resources for current analysis and as crucial elements for long-term observations of small bodies. Furthermore, such data enable the study of changes in activity over time and provide essential context for understanding evolutionary processes.
Various research methods for studying small bodies will be discussed, with the use of data from new space missions and modelling techniques contributing to a more accurate understanding of the mechanisms behind their activity, as well as to the development of new approaches to studying the origin and evolution of small bodies in the Solar System.

More than ten thousand tons of extraterrestrial objects, ranging in size from a few microns to a few meters in diameter, enter Earth’s atmosphere annually. A small fraction of these objects yields free samples of extraterrestrial matter—meteorites—for laboratory study. The majority of these objects burn up or ablate completely in the Earth’s atmosphere, appearing as visible meteors in the night sky. By recording meteor activity, recovering meteoritic material, and modeling the processes of atmospheric entry, ablation, and fragmentation, we can directly measure the flux, physical properties, and compositional diversity of small planetary impactors. The rapid advancement of observational, modeling, and analytical techniques has elevated meteoritical science to one of the primary avenues for investigating the nature and origin of interplanetary matter and its parent bodies. This session aims to serve as a platform for presenting fundamental results and innovative concepts spanning atmospheric observations, numerical modeling, meteorite recovery, and laboratory-based geochemical and physical characterization of impacting object remnants. In doing so, the session seeks to foster interaction across distinct communities and to highlight the interdisciplinary impact of ongoing and future research efforts within the broader planetary science framework.

Planetary regoliths play a key role in shaping the evolution, mechanical response, and exploration of celestial bodies across the Solar System. Understanding the behaviour of regolith materials in varying gravitational, thermal, and atmospheric conditions is essential for interpreting surface processes, understanding planetary origin and evolution, and for supporting future robotic and human exploration.
This session focuses on the mechanical, geotechnical, dynamical (flow) and thermophysical properties of regolith on planetary bodies such as the Moon, Mars, asteroids, comets, and natural satellites. We welcome contributions based on laboratory experiments, numerical simulations, and theoretical analyses, in addition to studies using in-situ, remote sensing, or returned sample data and simulants.
The session aims to provide a forum for advancing our understanding of regolith physics across planetary environments and for enhancing connections between disciplines: planetary science, granular physics, and geotechnical engineering. Interdisciplinary approaches that bridge experiments, modelling, and observations are encouraged and we particularly encourage early career scientists to submit an abstract for an oral presentation.

The section "Advances in Photopolarimetry and Spectropolarimetry of Solar System Small Bodies" highlights recent progress and breakthroughs in the application of these techniques to study small bodies, including asteroids, comets, moons, trans-Neptunian objects, and interplanetary dust. Photopolarimetry and spectropolarimetry provide critical insights into surface textures, particle sizes, porosities, and compositions, offering constraints on the physical, compositional, and dynamical evolution of these objects. We welcome abstract submissions on advancements in observational, numerical, and laboratory techniques, as well as innovative approaches for extracting and analyzing data, including new methodologies in photometric, polarimetric, and spectropolarimetric observations, advances in modeling, data reduction algorithms, and analysis pipelines, including machine learning, laboratory measurements of optical, polarimetric, and scattering properties, and software or web-based tools for collaborative data sharing and interpretation. This section aims to foster interdisciplinary discussions and encourage novel approaches that enhance our understanding of the physical properties, activity, and evolution of small bodies in the Solar System.

The goal of this session is to cover numerical simulations, artificial intelligence techniques and relevant laboratory investigations related to the Small Bodies (comets, KBOs, rings, asteroids, meteorites, dust), their formation and evolution, and the instruments of their exploration. This session is specially focused on the interdisciplinary approach in the development of models (formal descriptions of physical phenomena), experiments (on ground and in micro-gravity), artificial intelligence techniques (particularly machine learning) and mathematical simulations (computational methods and algorithms of solution) of various astrophysical phenomena: (i) dusty gas cometary atmospheres; (ii) volcanic activity on icy satellites (e.g. Enceladus and Io); (iii) planetary body formation (e.g. via pebbles growth), and planetesimal dynamics.

This session will include an introduction and discussion of new and/or existing laboratory studies in simulated space-like environments and models, experimental techniques, computational methods that can address the results of analytical, experimental and numerical analysis (with respect to computational methods and algorithms of solution) on the above described studies.

Abstracts on thermophysical evolution models of small bodies interiors as well as on the modeling of atmosphere and exosphere are welcome.

Asteroids preserve a record of the formation and evolution of the Solar System, encoded in their composition and physical properties. Over the past decades, significant progress has been achieved through a combination of telescopic observations, laboratory analyses of meteorites, and in-situ measurements by space missions. These complementary approaches provide critical constraints on asteroid mineralogy, surface processes, internal structure, and evolutionary pathways. The aim of this session is to bring together observational and experimental studies addressing the composition and physical characteristics of asteroids across different populations.