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Extension of the Newtonian creep tide theory to the spatial case.

Grant number: 19/11276-3
Support type:Scholarships abroad - Research Internship - Post-doctor
Effective date (Start): September 01, 2019
Effective date (End): August 31, 2020
Field of knowledge:Physical Sciences and Mathematics - Astronomy - Positional Astronomy and Celestial Mechanics
Principal researcher:Sylvio Ferraz de Mello
Grantee:Hugo Alberto Folonier
Supervisor abroad: Gwenael Boue
Home Institution: Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG). Universidade de São Paulo (USP). São Paulo , SP, Brazil
Research place: Observatoire de Paris, France  
Associated to the scholarship:16/20189-9 - Dynamic evolution due to tide in differentiated exoplanets and satellites, BP.PD


This project has as purpose to extend the creep tide theory to the spatial problem, that is,when the axis of rotation of the body deformed by the action of the tide is not perpendicularto the orbital plane. The Newtonian Creep tide theory (or Creep tide theory) developed at theIAG-USP, is a new reophysic tide theory that takes into account the nature (viscosity) ofobjects (Ferraz-Mello, 2013; 2015). Recently, this theory was reformulated by Folonier et al.(2018), simplifying the mathematical formalism of the original approach, and extended tothe case of differentiated bodies (Folonier and Ferraz-Mello, in preparation). The resultsobtained for Encélado and Mimas has shown that the new approach to creep has resulted ina very effective way to reproduce the available high-quality observational data obtained bythe CASSINI mission. However, due to the current state of the theory, its application isreduced only to the study of problems where the axis of rotation results perpendicular to theplane of the orbit. In this work, we intend to introduce improvements in the development ofthe theory and extend it to the many real star-planet and satellite-planet systems whosedynamic evolution can be directly affected by the inclination of the rotational axes of thebodies in relation to the relative orbital motion plane.

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