Long-term effect of the masses (and their uncertainties) of large asteroids on the...
Application of the planetary tides theory to exoplanets and planetary satellites
Capture, permanence and escape of resonances in the Solar System
| Grant number: | 14/02013-5 |
| Support Opportunities: | Scholarships in Brazil - Post-Doctorate |
| Effective date (Start): | August 01, 2014 |
| Effective date (End): | October 31, 2017 |
| Field of knowledge: | Physical Sciences and Mathematics - Astronomy - Positional Astronomy and Celestial Mechanics |
| Acordo de Cooperação: | Coordination of Improvement of Higher Education Personnel (CAPES) |
| Principal Investigator: | Rodney da Silva Gomes |
| Grantee: | Rogerio Deienno |
| Host Institution: | Instituto Nacional de Pesquisas Espaciais (INPE). Ministério da Ciência, Tecnologia e Inovações (Brasil). São José dos Campos , SP, Brazil |
| Associated scholarship(s): | 15/18682-6 - Late instability in the solar system, BE.EP.PD |
Abstract It is commonly accepted that the Asteroid Belt was formed by the partial agglutination of solid material available in that region, which was halted before the formation of a planet, due to the simultaneous appearance of Jupiter. However, for a more complete understanding of the scenario of asteroids formation, one must also take into account their characteristics and implications for the rest of the Solar System. Some of the most striking features of the Asteroid Belt are the mixture of physical properties among its component objects, as well as its peculiar distribution of orbital eccentricities and inclinations. Formation models of the Asteroid Belt notice that their formation is strongly linked to the size of the planet Mars, which is formed systematically larger than the actual planet. Walsh et al. (2011) show a possible solution to the impasse "size of Mars" vs "origin of the Belt" (their main focus). They also present plausible hypotheses for understanding the mixture of physical properties of the Belt objects. Regarding the orbital distribution of these objects, Walsh et al. (2011) achieve good agreement with the inclinations, but fail in relation to the eccentricities (very high). Moreover, after its formation, it is accepted that the asteroidal region still experienced the Late Heavy Bombardment (LHB). This in turn can change some of the properties already acquired by the Belt. In this paper, we assess the evolution of the orbital characteristics obtained in Walsh et al. (2011) until the LHB. During the LHB, we study the perturbations exerted by the planets on the Belt and the efficiency of the deposit of cometary objects in the asteroidal region. With this, we hope to be able to better understand the formation and orbital evolution of the Asteroidal Belt under a dynamical point of view, and as a consequence, of other features of the Solar System, trying to answer important yet unsolved questions. (AU) | |
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