Analysis of orbits for scientific missions around natural celestial bodies
Orbits of artificial planetary satellites in the neighborhood of the critical incl...
Grant number: | 12/12539-9 |
Support Opportunities: | Scholarships in Brazil - Master |
Start date: | September 01, 2012 |
End date: | February 28, 2014 |
Field of knowledge: | Physical Sciences and Mathematics - Astronomy - Positional Astronomy and Celestial Mechanics |
Principal Investigator: | Rodolpho Vilhena de Moraes |
Grantee: | Josué Cardoso dos Santos |
Host Institution: | Faculdade de Engenharia (FEG). Universidade Estadual Paulista (UNESP). Campus de Guaratinguetá. Guaratinguetá , SP, Brazil |
Associated research grant: | 11/08171-3 - Orbital dynamics of minor bodies, AP.TEM |
Abstract The aim of this project is the elaboration of theories and computer programs that will be used in aerospace missions concerning to the stability of orbits of artificial satellites around planetary satellites. The project refers to the translational motion of natural and artificial celestial bodies, taking into account perturbations by polygenic forces, such as, perturbations due the non-uniform distribution of the mass of the central body and the gravitational attraction by a third body.The equations of motion will be treated in closed form to avoid expansions in power of eccentricity and inclination. A canonical formalism will be described using the Delaunay variables. The set of canonical equations, which is a system of non-linear differential equations, will be used to study the stability of orbits around planetary satellites (Moon, Europe, asteroids, etc.). For Moon's satellites it will be used a simplified dynamical model which considers the effects produced by the non-sphericity of the Moon (J2-J9 and C22) and the gravitational attraction by the Earth. Emphasis will be given for frozen orbits that are orbits maintaining eccentricity, inclination and argument of perigee almost constant.The approach to study the stability of frozen orbits will done using the normal form for the Hamiltonian. | |
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