Abstract
The stability evolution of family f of the planar circular restricted three-body problem in the Earth–Moon case is explored numerically using the Poincare surface of section. It is shown that third order resonances are the main cause of the reduction of the stability region of retrograde satellites. Several branches of family f are also computed and these are seen by the configuration of their family characteristics to roughly determine the stability region. Previous results on smaller mass ratios of primaries are thus extended to the Earth–Moon system.
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