Hill's stability of the Moon in the spatial elliptic restricted three-body problem

Details Hill's stability of the Moon in the spatial elliptic restricted three-body problem Hill's stability of the Moon in the spatial elliptic restricted three-body problem

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005padeu..15..231m&link_type=abstract

In: Proceedings of the British-Romanian-Hungarian N+N+N Workshop for Young Researchers on Plasma- and Astrophysics: from laborat

Astronomy and Astrophysics

Astrophysics

Scientific paper

Hill's global and nonlinear stability theory has the advantage of being applicable to a great variety of dynamical systems, including those occurring in the solar system. He used his method originally to study the stability of the Moon as influenced by the Earth and the Sun. V. Szebehely showed that in the model of circular restricted three-body problem the measure of stability for the Earth's Moon is very low. Using the invariant relation of the spatial elliptic restricted three-body problem we show that the measure of stability for the Earth's Moon oscillate above stability critical value.

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