Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.231...85d&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 231, March 1, 1988, p. 85-95.
Astronomy and Astrophysics
Astronomy
8
Binary Stars, Eccentric Orbits, Orbit Perturbation, Stellar Mass, Three Body Problem, Circular Orbits, Companion Stars, Orbital Elements, Stellar Orbits, Stellar Systems
Scientific paper
The stability of low-mass binary systems moving on elliptical orbits in the presence of a large third mass is discussed in terms of three-body zero velocity surfaces. A closed form of solution is found which enables ranges of possible orbital elements to be determined for hierarchically stable systems. It is found that the ranges of stability decrease as the binary/third body mass ratio decreases for both prograde and retrograde systems. Systems with binary components of comparable mass are found to be more stable than those with differing masses. The eccentricity of the binary pair relative to the third body has a large effect on the stability of the system while the orbital eccentricity of the binary itself has only a minimal effect. Configurations moving on circular orbits are found to be the most stable and prograde systems are more stable than retrograde systems.
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