The Rosetta mission, led by the European Space Agency (ESA), aimed to study the comet Churyumov-Gerasimenko (67P) through remote sensing and in situ measurements. The spacecraft entered orbit around 1 the comet and collected data about its environment and structure.

The mission tracked the evolution of the comet along its trajectory, studying changes in its activity before, during, and after its closest approach to the Sun, and concluded with a controlled landing on the comet’s surface1. Comets are considered time capsules containing material from our Solar System’s early stages. These small bodies, where temperatures are low, are understood to be the least processed bodies in the Solar System, offering a unique insight into the planetary formation. Preusker et al. [1] determined the total volume of the nucleus as approximately 18.7 km3 by extrapolation from the volume of the comet’s northern hemisphere. P¨atzold et al. [2] presented the determination of the mass, average density, and internal structure of the nucleus of comet 67P, based on the analysis of its gravitational field derived from the probe’s radio science data. Vallat et al. [3] described in detail the scientific planning process of the mission, from the conditions of the planning of operations, such as thermal constraints, limitations of solar energy generation, gas drag forces, to the orbital conditions resulting from the gravity of its irregular nucleus. Recent studies have examined the connection with surface behaviors and topographic features of celestial bodies like (101955) Benu, (486958) Arrokoth, Ryugu, and (3200) Phaethon, from dynamical characteristics such as geopotential surface, slopes, escape speed, and equilibrium points [4–9]. Scheeres et al. [4] investigated dynamical features on Bennu’s surface and found that particles near the pole could reach velocities that would remain below the asteroid’s escape speed. Amarante & Winter [6] studied the dynamics of the KBO Arrkoth and identified that the equatorial regions of the two lobes of the contact binary act as geopotential maxima and maintain their surface acceleration between 0.5 and 1 mm s−2. Amarante et al. [5] found that large particles could collide with the surface of Bennu at low speeds, preferably in high latitude regions, close to the equator, and also to the north pole of the asteroid. In contrast, areas of latitude would be less populated. Fu et al. [8] identified six external equilibrium points, located along the ridge of Ryugu, and also analyzed their topological stability. They also mapped the families of symmetric periodic orbits associated with these points, identifying 15 families, some of which converge to other equilibrium points. In contrast, others end on the surface of Ryugu, and one of them exhibits a cyclic behavior throughout its evolution. Jo et al. [9] analyzed the dynamic environment near the asteroid Phaethon, to support JAXA’s DESTINY+ mission, determining several dynamic properties of its surface from its geopotential, such as the escape speed at its surface, which is approximately 1 m s−1.
They also found seven equilibrium points, one of which is linearly stable, and the others are all unstable. Hasselmann et al. [10] analyzed the Khonsu region, in the southern hemisphere of the comet 67P, also through images provided by the OSIRIS instrument. This region showed intense activity during the comet’s pericenter passage. Moreno et al. [11] examined the rotational dynamics of irregularly shaped cometary particles, considering the combined effects of gas drag and radiative forces and torques. Their model applied to comet 67P revealed that radiative torques were negligible compared to gas-driven torques for particles larger than 10 µm. Frattin et al. [12] focused on the motion of dust particles in the inner coma of 67P, analyzing OSIRIS images to study the trajectories, rotation, and size of the particles. Their results showed that the particles were slow rotators, did not undergo fragmentation, and provided valuable parameters for improving dynamical models of the cometary coma. Lemos et al. [13] characterized large aggregates (≥1 cm) from comet 67P. They determined that the aggregates had an average radius of approximately 5 cm and mapped their source regions near terrain boundaries on the comet’s surface, considering the mascon model [14]. Czechowski & Kossacki [15] examined material ejected from the Hatmehit depression on comet 67P, modeling the ejecta with various initial velocities using the mascon model. Finally, Scheeres [16] calculated the location and stability of equilibrium points around comet 67P using the mascon model approach. They found four unstable equilibrium points around comet 67P.
1https://www.esa.int/Enabling Support/Operations/Rosetta In this work, we analyze in detail the surface dynamics and the orbital dynamics of comet 67P/Churyumov-Gerasimenko from an adequate 3-D polyhedral shape model2 obtained by [17].