Stability of inner planetary systems

Details Stability of inner planetary systems Stability of inner planetary systems

Mar 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979zamp...30..364s&link_type=abstract

Zeitschrift für angewandte Mathematik und Physik, vol. 30, Mar. 25, 1979, p. 364-369. NSF-NATO-NASA-supported research.

Astronomy and Astrophysics

Astronomy

Celestial Mechanics, Planetary Systems, Planets, Solar Orbits, Systems Stability, Three Body Problem, Astronomical Models, Motion Stability, Natural Satellites, Solar System

Scientific paper

The stability of inner planetary systems with arbitrary mass ratios is studied on the basis of the model of the plane restricted three-body problem. A quantitative stability criterion is obtained in terms of the difference between the critical value of the Jacobi constants (at which bifurcation can occur) and the critical value corresponding to a planetary orbit. An orbit is stable if it cannot leave a region that contains only the larger central body (Hill). For small values of the mass parameter, the maximum dimensionless radius of a Hill-stable orbit is 1 minus 2.4 times the cube root of the mass parameter.

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