On the stability of the inner planets, satellites and close binaries

Details On the stability of the inner planets, satellites and close binaries On the stability of the inner planets, satellites and close binaries

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982cha%26a...6..267z&link_type=abstract

Chinese Astronomy and Astrophysics, Volume 6, Issue 3, p. 267-272.

Astronomy and Astrophysics

Astrophysics

Scientific paper

I consider the range of Hill stability in the restricted circular problem of three bodies when the larger one of the two principal bodies has a finite oblateness. I show that the range r satisfies the equation r = 1- μ/Ccr - 3μ + μr2 - v (1- μ)r-3 +/-(2 + 3v)√(1 - μ (1 + 3v/r2)r, where μ is the mass parameter and v is an oblateness parameter. This result is applied to the solar system, the Earth-Moon system and binary star systems. It is then shown that, all the inner planets of the solar system, the great majority of asteroids and some short-period comets are Hill stable, that direct artificial satellites of the Earth are more stable than retrograde ones, and that contact binaries possess cores between which no mass exchange takes place.

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