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We calculate the location and stability of the L_4 and L_5 Lagrangeequilibrium points in the circular restricted three-body problem as the binarysystem evolves via gravitational radiation losses. Relative to the purelyNewtonian case, we find that the L_4 equilibrium point moves towards thesecondary mass and becomes slightly less stable, while the L_5 point moves awayfrom the secondary and gains in stability. We discuss a number of astrophysicalapplications of these results, in particular as a mechanism for producingelectromagnetic counterparts to gravitational-wave signals.

The Lagrange Equilibrium Points L_4 and L_5 in a Black Hole Binary System