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| Author(s): |
Rafael Ribeiro de Sousa
Total Authors: 1
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| Document type: | Doctoral Thesis |
| Press: | Guaratinguetá. 2019-09-11. |
| Institution: | Universidade Estadual Paulista (Unesp). Faculdade de Engenharia. Guaratinguetá |
| Defense date: | 2019-09-05 |
| Advisor: | Ernesto Vieira Neto; Rodney da Silva Gomes; Alessandro Morbidelli |
| Abstract | |
A study of the formation and evolution of the Solar System is a source of information for an understanding of what conditions life could arise and evolve. We present a numerical study of the final stage of accretion of the giant planets of the Solar System during and after the protoplanetary gas disc phase. In our simulations, we use a recent and reliable model for the formation of Uranus and Neptune to sculpt the properties of the original trans-Neptunian disk (Izidoro et al. , 2015a). We have done this study in a self-consistent way considering the effects of gas and the evolution of planetary embryos which form Uranus and Neptune by mutual giant collisions. We considered different Jupiter migration stories due to the uncertainty of how Jupiter’s migration was during the gas phase. Our simulations provide for the first time to obtain the orbital properties of the original trans-Neptunian disk. We then calculate the instability time of the giant planets from planetary systems which form similar Uranus and Neptune. Our results strongly indicate that the instability of the giant planets occurs early within 500 million years and even more likely to happen at 136 million years after gas dissipation. We also perform simulations to discuss some dynamical effects that happen in the Kuiper belt region. These effects happen when Neptune was in high eccentricity during planetary instability. For this problem, we use the simulations performed by Gomes et al. (2018) who investigated the compatibility of the Kuiper cold belt formation in the latest Nice model framework. Cold population production takes place in situ in Gomes et al. (2018) with planetesimal disc extended to 45 AU. The simulations of Gomes et al. (2018) have shown good results but some Neptune evolutions are too drastic to obtain low eccentricities which are present in the current Kuiper belt. We perform simulations for the production of the cold population in the face of a phase that is most drastic for the cold population’s retention: the eccentric phase of Neptune (e > 0.2) and the slow precession of the perihelion longitude of this planet (Batygin et al. , 2011). We performed new simulations but considering the mutual interaction of objects (self-gravity) with the size of a few pluto, or smaller, embedded in the Kuiper belt. With these results, we can see if the dispersion caused by the self-gravity is capable of producing lower eccentricity objects during the violent phase of Neptune. We also apply secular theory to explain our results. The planetesimals reach low eccentricities with the self-gravity but considering a more massive disk than the observed Kuiper belt. Therefore, we conclude that the ideal for Neptune’s evolution to produce the cold population even at high eccentricity is the synchronism between the secular cycles of the planetesimals and the duration of Neptune’s eccentric and slow precession phase. (AU) | |
| FAPESP's process: | 15/15588-9 - The stability of the solar system dynamical evolution via Nice Model |
| Grantee: | Rafael Ribeiro de Sousa |
| Support Opportunities: | Scholarships in Brazil - Doctorate |