The stability of binary star systems during encounters with a third star

Details The stability of binary star systems during encounters with a third star The stability of binary star systems during encounters with a third star

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.210..915d&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 210, Oct. 15, 1984, p. 915-927.

Astronomy and Astrophysics

Astronomy

13

Binary Stars, Motion Stability, Orbital Elements, Stellar Motions, Three Body Problem, Eccentric Orbits, Numerical Integration, Stellar Mass

Scientific paper

The interaction of a binary star system and a third star not moving on a closed orbit is discussed in terms of three-body zero velocity surfaces. The ranges of orbital parameters for which the binary system is stable against disruption or collision by a third star moving on a parabolic or hyperbolic orbit are determined. It is found that the regions of stable motion decreased as the mass and eccentricity of the passing star increased.

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