Hill's stability in the elliptic restricted three-body model including body shape

Details Hill's stability in the elliptic restricted three-body model including body shape Hill's stability in the elliptic restricted three-body model including body shape

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982acasn..23..390h&link_type=abstract

(Acta Astronomica Sinica, vol. 23, no. 4, 1982, p. 390-397) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 7, June 19

Astronomy and Astrophysics

Astrophysics

Elliptical Orbits, Hill Method, Orbit Perturbation, Planetary Orbits, Solar Orbits, Three Body Problem, Eccentric Orbits, Natural Satellites, Orbital Mechanics

Scientific paper

It is shown that the inclusion of the J2-term of the planet and its orbital eccentricity may alter the stability character of a satellite in the sense of Hill. The effect depends on the initial conditions. With the actual initial conditions, the satellite S9 is Hill stable, whether or not these terms are considered, but if S9 were located at a distance of 330 Saturn radii, then it would be unstable or stable depending on whether or not these terms are considered.

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