Be interacting binaries have also benefit from high angular resolution observations. In the paper by Harmanec et al. 1996, they confirm the spatial orientation of the projection of the vector of the orbital angular momentum on the sky (theta = 160° from the North). Moreover, interferometric, spectroscopic, photometric and polarimetric data confirm that the bulk of the Hα and HeI 6678 emission seems to originate from jets perpendicular to the orbital plane. These jets are associated with the more massive (primary) component of the binary. They may originate from a "hot-spot" in the disk where the gas stream is flowing through the Roche lobe of the second component (B6-8 II) toward the primary. It seems that some contribution to the emission may also comes from an intermediate region between the two stars. This result agrees well with the analysis of UV line polarization.
The results of that campaign are in: Harmanec, P., Morand, F., Bonneau, D., Bozic, H., Guinan, E.F., Hadrava, P., Hall, D.S., Jiang, Y., Mourard, D., Stee, Ph., Sterken, C., Tallon-Bosc, I., Vakili, F., Walker, G.A.H., Yang, S. and Le Contel, J.M. 1996, "Jet-like structures in β Lyr?", A&A, 312, 879
Here is a picture showing how this binary system is supposed to be:
