| Grant number: | 21/07181-7 |
| Support Opportunities: | Scholarships abroad - Research Internship - Doctorate |
| Start date: | November 01, 2021 |
| End date: | August 31, 2022 |
| Field of knowledge: | Physical Sciences and Mathematics - Astronomy - Solar System Astronomy |
| Principal Investigator: | Silvia Maria Giuliatti Winter |
| Grantee: | Gustavo Oliveira Madeira |
| Supervisor: | Sébastien Charnoz |
| Host Institution: | Faculdade de Engenharia (FEG). Universidade Estadual Paulista (UNESP). Campus de Guaratinguetá. Guaratinguetá , SP, Brazil |
| Institution abroad: | Institut de physique du globe de Paris, France |
| Associated to the scholarship: | 18/23568-6 - Scenarios for the formation of Neptune's arcs and the giant satellites of the Solar System, BP.DR |
Abstract JAXA's Martian Moon eXploration (MMX) mission is expected to arrive on the Mars system in 2023 for a complete observational and geological study of the martian system. The mission, which will also collect samples of the moon Phobos, aims to answer the main question: How did the martian moons, Phobos and Deimos, form? Formation models propose the formation of these moons in a debris disk generated in a giant impact from an exterior impactor with Mars. In this scenario, the impact material settles on a circular and equatorial disk almost completely within the Roche limit of Mars. The outwards viscous spreading of the disk material allows the formation of porous satellites (rubble-pile type) at the Roche limit of the planet. Thus, due to an intricate balance between outward migration caused by disk-moon interaction and inward migration caused by martian tides, satellites are believed to be continually destroyed and recreated at the Roche limit due to tidal effects. Phobos and Deimos would correspond to the latest generation of these. In this work, we intend to analyze through dynamic considerations the validity of this scenario and its implications in the composition of Phobos and in the martian system in general. We will carry out numerical simulations of a rubble-pile satellite of different compositions right at the Roche limit of the planet under the effects of the martian tides, checking if the satellite is indeed destroyed. We will track the evolution of the destruction material and if it falls on the planet trying to answer the question about the fate of the debris disk and the non-observation of rings around Mars (and also the traces caused by the material on Mars surface). The chemical composition of the satellites formed by the regrouping at the Roche limit will be analyzed. The study is proposed with the objective of obtaining constraints regarding the composition of the satellites and the Mars system. The project will be carried out in contact with the MMX team and our results will be used to help the design of the mission observations. (AU) | |
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