On the stability of close binaries in hierarchical three-body systems

Details On the stability of close binaries in hierarchical three-body systems On the stability of close binaries in hierarchical three-body systems

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983cemec..29..215w&link_type=abstract

Celestial Mechanics (ISSN 0008-8714), vol. 29, March 1983, p. 215-228. Research supported by the Science and Engineering Researc

Computer Science

7

Binary Stars, Celestial Mechanics, Hill Method, Mass Ratios, Orbit Decay, Systems Stability, Three Body Problem, Dwarf Stars, Galaxies, Giant Stars, Longitude, Natural Satellites, Planets, Rotation

Scientific paper

The Hill-type stability of general hierarchical three-body systems is examined analytically in the case where the total mass of the binary is small in comparison to the mass of the external body. This is compared with results derived by Szebehely, Markellos and Roy (1977, 1978, 1981) in the planet-satellite-sun case of the circular restricted three-body problem. It is demonstrated how the Hill-type stability is affected by the sense of revolution of the binary, i.e., corotational or contrarotational, and the mass ratio within the binary. The effect of the difference in longitudes of the bodies in their orbits is also examined.

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