  I propose that the relatively high eccentricity found in some tidally
strongly interacting binary systems, where the mass-losing star is an evolved
giant star, e.g., an asymptotic giant branch star, is caused by an enhanced
mass loss rate during periastron passages. Tidal interaction by itself will
circularize the orbits of these systems in a relatively short time, hence a
mechanism which increases the eccentricity on a shorter time scale is required.
The proposed scenario predicts that the nebula formed by the mass loss process
possesses a prominent departure from axisymmetrical structure. Such a departure
is observed in the Red Rectangle, which has a central binary system, HD 44179,
with an orbital period of 318 days, and an eccentricity of e=0.38.
