A simple, accurate, geometrical approximation to the Keplerian motion (Q911569)
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scientific article; zbMATH DE number 4141989
| Language | Label | Description | Also known as |
|---|---|---|---|
| English | A simple, accurate, geometrical approximation to the Keplerian motion |
scientific article; zbMATH DE number 4141989 |
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A simple, accurate, geometrical approximation to the Keplerian motion (English)
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1989
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The position of a body in Keplerian elliptical motion is determined with respect to the main axes by an angle called the eccentric anomaly, which depends on time in terms of a transcendental equation. The latter can be approximated by developing a series. The author interprets geometrically modifications of the series in order to improve its convergence. The article is meant for those interested in computing planetary positions and also for students of the early history of celestial mechanics.
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classical one-body-motion
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eccentric anomaly
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celestial mechanics
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0.88292265
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0.87814504
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0.87054825
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0.86734176
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0.85522765
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