Open AccessHill stability of a triple system with an inner binary of large mass ratio
Author(s) -
Brasser R.
Publication year - 2002
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2002.05330.x
Subject(s) - physics , dimensionless quantity , mass ratio , binary number , eccentricity (behavior) , lagrangian point , orbit (dynamics) , function (biology) , angular momentum , celestial mechanics , three body problem , astrophysics , classical mechanics , quantum mechanics , arithmetic , mathematics , engineering , evolutionary biology , political science , law , biology , aerospace engineering
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.