A stability condition for resonant rotations of celestial bodies

Details A stability condition for resonant rotations of celestial bodies A stability condition for resonant rotations of celestial bodies

Dec 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978azh....55.1308k&link_type=abstract

Astronomicheskii Zhurnal, vol. 55, Nov.-Dec. 1978, p. 1308-1312. In Russian.

Astronomy and Astrophysics

Astronomy

Celestial Mechanics, Rotary Stability, Rotating Bodies, Solar System, Differential Equations, Dynamic Models, Motion Stability, Planar Structures, Synchronism

Scientific paper

The rotational stability of a natural celestial body whose motion about its center of mass is synchronized with its mean orbital motion is investigated. A stability analysis is performed which reveals a possible reason why the majority of such synchronisms are not achieved in the solar system. Specifically, it is suggested that the quasi-planar structure of the solar system prevents most types of synchronous rotation because the angle between the rotational axis of most large solar-system bodies and the normal to their orbits is too large.

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