A bstract. The differential equations of motion for the restricted three-body problem have been integrated numerically to give the path (in a rotating frame of reference) of a particle ejected radially from one component of a close double star system. This has been done for several mass ratios and initial positions and velocities. The most usual results are a ring around one component rotating in a forward direction, or for higher velocities, a ring around both components rotating in a retrograde direction. A particle ejected from the first Lagrangian point will form an orbit only if the mass of the star from which it is ejected is approximately one-fifth or less that of its companion.