| Grant number: | 16/12113-2 |
| Support Opportunities: | Scholarships abroad - Research Internship - Doctorate |
| Effective date (Start): | September 01, 2016 |
| Effective date (End): | August 31, 2017 |
| Field of knowledge: | Physical Sciences and Mathematics - Astronomy - Solar System Astronomy |
| Principal Investigator: | Ernesto Vieira Neto |
| Grantee: | Ricardo Aparecido de Moraes |
| Supervisor: | Wilhelm Kley |
| Host Institution: | Faculdade de Engenharia (FEG). Universidade Estadual Paulista (UNESP). Campus de Guaratinguetá. Guaratinguetá , SP, Brazil |
| Research place: | Eberhard Karls Universität Tübingen, Germany |
| Associated to the scholarship: | 13/24281-9 - Study of the giant planet's satellites formation using bi-dimensional hydrodynamics numerical integration with star perturbation, BP.DR |
Abstract The formation of the regular satellites are one of the most intriguing problem of the astronomy, the physical effects that led such large bodies grows close to planets are not completely understood yet. One way to study the formation of those bodies is through numerical simulations. In the past few decades the number of computational tools for astronomy increase substantially, however the study of formation of satellites close to planets is still challenging, because the current numerical integrators does not provide high resolution in the regions were the satellites are believed to form. In this project we propose a new approach for this problem, once the satellite is forming close to the planet, the focus of the study is in the region of influence of the planet, in this way the effects that does not affect this region may be neglected. For this we remove the star from the center of the system and place the hosting planet as the central body, with this modification allow us to study regions close to the planet without loosing resolution and details, however this same modification will imply several simplifications on the problem, once the planet will not orbit any body, for example. This technique is not quite new and the major problem of this modification is the lack of inclusion of the effects due to the star, most of the previous papers that exchange the central star for a central planet did not add any factor to compensate the effects of the star, in our approach we add the effects of the star as a term in the gravitational potential this avoid the integration of the "trajectory"of the star around the central planet. As a complement of the work with satellites we expect to test our approach in binary systems, where the change in the central star is not needed, nevertheless is a good scenario to test our hypothesis of adding the effects, in this case, of the secondary star rather than integrating it. (AU) | |
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