Stability of outer planetary orbits (P-types) in binaries

Details Stability of outer planetary orbits (P-types) in binaries Stability of outer planetary orbits (P-types) in binaries

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...226..335d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 226, no. 1, Dec. 1989, p. 335-342.

Astronomy and Astrophysics

Astrophysics

35

Binary Stars, Celestial Mechanics, Extrasolar Planets, Orbital Mechanics, Planetary Orbits, Double Stars, Eccentricity, Stability, Three Body Problem

Scientific paper

The stability limits of fictitious planetary orbits around both components of a binary system is studied numerically, using the elliptic restricted three-body problem as a model. Two critical orbits are determined: the Upper Critical Orbit and the Lower Critical Orbit. Between these two limits, stable and unstable orbits are found. It is shown that the formula of Dvorak (1986) can be used to derive stability limits for fictitious planets on P-type orbits surrounding both primaries in direct orbits. This formula is applied to 17 double stars, showing that there could exist stable planetary orbits even in binaries. The orbital periods around the two bodies would be of the order from ten to a few hundred years.

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