  In this paper we analyze the impact of the boundary conditions on the
solutions of the $\gamma$-structure equations for magnetized Bose-Einstein
condensate stars (BECs). We consider two cases: a pure BECs and a BECs embedded
in a magnetic field. Since they correspond to different physical situations,
they lead to different numerical behavior, having important effects on the
stability of the solutions as well as on the observables of the star. The
differences between the mass-radii curves obtained in each situation are
presented and discussed.
