CONICET | Buscador de Institutos y Recursos Humanos

The late accretion stages of planetary formation is a topic that has been deeply studied during the last decades. One of the goals of these kind of studies, is the analysis of the water accretion processes in the framework of the terrestrial planet formation, in different dynamical formation scenarios. Most of the works that address this issue, resort to the development of N-body numerical simulations. However, due to the high computational cost that these types of simulations require, certain simplifications to reduce CPU time are usually considered. One of such simplifications is to reduce the total number of bodies, and another is to assume that the bodies representing planetesimals are not self-gravitating. This means that, although that the planetesimals interact gravitationally with the embryos population, they do not interact with each other. This phenomenon of self-gravity, which is in general not taken into account, can lead to significant changes in the water accretion processes of terrestrial planets located in the habitability zones, and their final water contents may be different. In this work, we show preliminary results on planetary formation using the GENGA code (Gravitational Encounters in N-body Simulations with GPU Acceleration), which is a N-body integrator based on the integration scheme of the Mercury code, widely used by the astronomical community, and in which all operations are performed in parallel, including the close encounter detection and the grouping of independent close encounter pairs. These advantages allow us to include self-gravity and also a larger number of objects in our simulations, aiming to better constrain the final water contents of the planets that remain within the habitable zones of different planetary systems architectures.