  In this article, equilibrium points and families of periodic orbits in the
vicinity of the collinear equilibrium points of a binary asteroid system are
investigated with respect to the angular velocity of the secondary body, the
mass ratio of the system and the size of the secondary. We assume that the
gravitational fields of the bodies are modeled assuming the primary as a mass
point and the secondary as a rotating mass dipole. This model allows to compute
families of planar and halo periodic orbits that emanate from the equilibrium
points $ L_1 $ and $L_2$. The stability and bifurcations of these families are
analyzed and the results are compared with the results obtained with the
Restricted Three-Body Problem (RTBP). The results provide an overview of the
dynamical behavior in the vicinity of a binary asteroid system.
