Hill stability of a triple system with an inner binary of large mass ratio

Details Hill stability of a triple system with an inner binary of large mass ratio Hill stability of a triple system with an inner binary of large mass ratio

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mnras.332..723b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 332, Issue 3, pp. 723-728.

Astronomy and Astrophysics

Astronomy

4

Stellar Dynamics, Celestial Mechanics

Scientific paper

We determine the maximum dimensionless pericentre distance a third body can have to the barycentre of an extreme mass ratio binary, beyond which no exchange or ejection of any of the binary components can occur. We calculate this maximum distance, q '/a , where q ' is the pericentre of the third mass to the binary barycentre and a is the semimajor axis of the binary, as a function of the critical value of L 2 E of the system, where L is the magnitude of the angular momentum vector and E is the total energy of the system. The critical value is obtained by calculating L 2 E for the central configuration of the system at the collinear Lagrangian points. In our case we can make approximations for the system when one of the masses is small. We compare the calculated values of the pericentre distance with numerical scattering experiments as a function of the eccentricity of the inner orbit, e , the mutual inclination i and the eccentricity of the outer orbit, e '. These show that the maximum observed value of q '/a is indeed the critical q '/a , as expected. However, when e '->1, the maximum observed value of q '/a is equal to the critical value calculated when e '=0, which is contrary to the theory, which predicts exchange distances several orders of magnitude larger for nearly parabolic orbits. This does not occur because changes in the binding energy of the binary are exponentially small for distant, nearly parabolic encounters.

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