Abstract:
The continuous development and upgrading of computational methods has allowed for great advances in scientific research in fields like astrophysics. The capacity of this methods to accurately reproduce processes and environments that can not be directly observed makes them specially useful in areas like planet formation, as the stages of planetary growth can be rarely observed and directly studied. From dust to planetesimals, protoplanetary embryos and terrestrial planets, planetary growth is still a field of open research, specially as many processes like the formation of planetesimals and the origin of water in terrestrial planets remains unclear. Specially for the origin of water a number of hypothesis have been postulated including both endogenous and exogenous sources, such that the most plausible source of the water accreted by the inner planets of the Solar System corresponds to bodies originated in the outer asteroid belt. The delivery of water is most likely carried out by massive and decisive collisions of similar sized bodies during the late-stage accretion phase of planetary growth. In this master thesis, the focus is placed on studying in detail this type of collisions, utilizing a post-collisional processing python code using the N-body integrator REBOUND, which determines a wide array of parameters for the resulting fragments, as final mass and number of collisions, while at the same time performing a gravitational analysis of the system in order to obtain gravitationally bound aggregates, their orbits and their respective orbital parameters. For a scenario consisting of four collisional events, initially performed by Burger et al. (2020), we obtain unique gravitational systems as a direct consequence of the different impact parameters presented by each collision of the scenario, where the impact angle has the greatest incidence on the outcome of the collision, such that scenarios with large grazing angles result in systems that are completely gravitationally bound, while scenarios with smaller straight-on angles result in systems with numerous fragments in independent trajectories. Additionally, from the analysis of the post-collisional system we obtain a protoplanetary embryo with a growth path consistent with a viable candidate for a terrestrial planet in the Solar System, presenting a final stable co-planar circular orbit located in the habitable zone.
Citación recomendada (normas APA)
Daniela Muñoz Giraldo, "Analysis of fragment dynamics and collisional evolution after similar sized collisions during terrestrial planet formation", Colombia:-, 2021. Consultado en línea en la Biblioteca Digital de Bogotá (https://www.bibliotecadigitaldebogota.gov.co/resources/3711737/), el día 2025-05-12.
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