Abstract
The orbital motion around a central body is an interesting problem that involves the theory of artificial satellites and the planetary theories in the solar system. Nevertheless some difficult situations appear while studying this apparently simple problem, depending on each particular case. The real problem consists of searching the perturbed solution from a basic two-body motion problem. In addition, the perturbed problem must be solved using a numerical method and its efficiency depends on the selected coordinate system and the corresponding time. In fact, local and global errors are not necessarily homogeneously distributed over the orbit. In other words, there is a strong relationship between the spatial distribution of the selected points and the temporal independent variable. This is particularly dramatic in specially difficult cases. This issue leads us to consider different anomalies as temporal variables, searching for both precision and efficiency. Therefore, we are interested in the study of techniques to integrate the orbital motion equations using different anomalies as temporal variables which are functions of one or more parameters. The final aim of this paper is the minimization of the integration errors using an appropriate choice of the parameter depending on the eccentricity value in the family of the generalized Sundman anomalies.
Highlights
One of the most important problems in spatial mechanics is the study of the motion of an artificial satellite around the Earth
The generalized family of Sundman anomalies is adequate to be used in the numerical integration of the perturbed twobody problem
To study the optimal value of α in order to increase the performance of the numerical methods, we have carried out some numerical experiments on the unperturbed two-body problem
Summary
Our interest lies in being able to integrate the not disturbed problem, whose exact solution (in a formal and closed form, including series, integrals, and implicit equations) is known, by means of a method that allows reducing the errors using the maximum norm, both for the position and for the velocity. With this aim, we know that a bad distribution of the points in the periapsis and the apoapsis leads inexorably to truncation errors of such magnitude that make impossible the task proposed regarding the reduction of errors. We expose the main conclusions and remarks about this paper
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