Deimos is only one of two small moons orbiting Mars, alongside the larger and more irregular Phobos. Its origin has remained difficult to establish because its dark, subdued surface can be consistent with more than one history. The moons could have formed from material thrown into orbit after a massive impact on Mars, developed from debris left over from the planet’s formation, or been captured asteroids that became gravitationally bound to the Red Planet. Each scenario must account for the moons’ shapes, surfaces, orbits and likely compositions. Deimos is particularly challenging because it is relatively smooth compared with the heavily cratered, fractured bodies commonly associated with violent collisions. A formation model therefore has to explain not only how the moon acquired its mass, but also why its surface looks as if it was blanketed and gently reworked rather than simply battered by countless impacts.

The new work focuses on a “subcatastrophic” impact, a collision that dramatically modifies a target without completely dispersing it. In the simulations, the impact is oblique rather than head-on. That geometry matters because an angled strike can excavate material from one region, redistribute it across the target and alter the body’s shape while leaving much of the original object gravitationally bound. The calculations show that such an event can reproduce Deimos’s broad form and generate a prominent depression near its south pole. Rather than treating the depression as an unrelated feature formed later, the model connects it directly to the moon’s transformation. The collision would have transferred energy and momentum into Deimos, deforming its surface and mobilizing a large volume of loose material. As the debris settled, it could have smoothed older topography and produced the relatively subdued appearance that distinguishes Deimos from many other small Solar System bodies.

The key physical process is the competition between impact energy and self-gravity. On a small moon such as Deimos, gravity is weak enough that excavated fragments can travel substantial distances across the surface, yet strong enough to draw a fraction of the debris back after the collision. Material accelerated above the surface would follow ballistic trajectories: it would rise, arc through the surrounding space and return under Deimos’s gravitational pull. Some particles could also escape entirely, but the simulations indicate that enough would remain available to coat the moon. This fallback regolith would act like a geological blanket, filling low areas, covering exposed blocks and damping the sharp relief produced by the initial strike. The result is not a perfectly uniform sphere, but a reshaped, mantled body in which the impact scar remains visible while much of the surrounding terrain appears smooth.

The simulations also point to an interior unlike that of a solid, monolithic rock. Deimos may instead have a structure comparable to a rubble-pile asteroid: a gravitationally bound collection of fractured rocks, porous material and loose particles, with substantial empty space between components. Such bodies can absorb and redistribute impact energy differently from solid blocks. They may deform, compact or rearrange internally without behaving like a single piece of rock. The low-strength surface observed on the near-Earth asteroid Ryugu provides an important comparison for this kind of behavior. Experiments involving an artificial impact on Ryugu showed how a weak, rubble-rich asteroid can develop a crater under conditions governed largely by gravity rather than by the strength of intact rock. The Deimos simulations apply related physical reasoning to a Martian moon, suggesting that its response to an impact could have involved widespread movement of granular material rather than simple fracturing of a rigid crust.

Reconstructing Deimos’s shape is central to the argument. The study uses a high-resolution shape model derived from stereophotoclinometry, a technique that combines images taken under different illumination and viewing conditions to estimate surface slopes and three-dimensional relief. By comparing simulated post-impact bodies with this reconstructed shape, the researchers tested whether a single collision could generate the moon’s major geometric features. The result described in the research briefing is that an oblique impact can reproduce two of Deimos’s most defining characteristics at once: its overall form and its smooth surface. A model that matches only one feature would provide limited evidence, because many different processes can produce a depression or a rounded silhouette independently. Matching both suggests that the observed geology may be physically linked. The moon’s shape is therefore being treated not merely as a visual curiosity, but as a constraint on its origin.

The proposal is significant because it could connect Deimos to a broader population of small bodies that formed through collisions and subsequent gravitational reassembly. In the early Solar System, impacts were common, and many objects may have experienced repeated cycles of fragmentation, reaccretion and surface burial. A collision that reshaped Deimos without destroying it could have left the moon with a mixed history: an older interior inherited from its precursor and a younger exterior assembled from impact-generated debris. That interpretation would help explain why the moon may retain an asteroid-like internal architecture while displaying a surface that is comparatively smooth. It also illustrates why the appearance of a small planetary body can be misleading. A calm-looking exterior does not necessarily indicate a gentle origin; it may instead record the final stage of a violent event, after debris settled and erased much of the immediate evidence of disruption.

The findings also reopen questions about the relationship between Deimos and Phobos. The two moons share the same planetary neighborhood, but their geological histories may not be identical. Competing formation scenarios have long attempted to explain both satellites together, while observations suggest that their shapes and surfaces contain important differences. A model that works for Deimos must therefore be tested against the broader Martian system rather than accepted as a universal explanation for both moons. If Deimos’s smoothness and south-polar depression were produced by one oblique impact, Phobos may have experienced a different collision history, a different internal structure or a different degree of regolith redistribution. Alternatively, the two moons could still share a common origin while diverging later because of variations in size, composition, porosity and impact angle. Their similarities and contrasts may ultimately reveal how small moons evolve after formation.

Future observations could provide the decisive test. Japan’s Martian Moons Exploration mission is designed to investigate the Martian satellite system, with close observations of the moons and the return of samples from Phobos planned to illuminate their formation. Although the mission’s returned material would come from Phobos rather than Deimos, measurements of both moons’ surfaces, shapes, densities and geological features could test whether they possess the asteroid-like characteristics predicted by impact and rubble-pile models. For Deimos, particularly valuable evidence would include detailed mapping of the south-polar depression, measurements of surface texture and composition, and improved constraints on its mass and internal density distribution. If the moon’s exterior consists of impact-fallback debris, its mineralogy and particle-size distribution may differ from material exposed in deeper regions. If its interior is porous and loosely assembled, its response to gravity, rotation and thermal evolution should also carry detectable signatures.

The new scenario does not close the case on Deimos’s origin, but it gives researchers a coherent explanation for features that previously required separate geological stories. One collision could have carved the moon’s polar depression, rearranged its body, scattered material across its surface and left behind a porous interior resembling that of a rubble-pile asteroid. The idea is compelling precisely because it links form, surface texture and internal structure through a single physical event. It also transforms Deimos from a small, enigmatic satellite into a potential fossil of planetary violence. As spacecraft return to the Martian system and improve measurements of its moons, the smooth little body may reveal whether its appearance is the product of quiet accretion, ancient capture or one extraordinary impact that changed it forever.