  We show that substantially enhanced mass loss at periastron passages, as is
expected in the grazing envelope evolution (GEE), can compensate for the
circularization effect of the tidal interaction in binary systems composed of
an asymptotic giant branch (AGB) star and a main sequence secondary star. By
numerically integrating the equations of motion we show that under our
assumptions the binary system can maintain its high eccentricity as the AGB
star evolves toward the post-AGB phase. Our results can explain the high
eccentricity of some post-AGB intermediate binaries (post-AGBIBs), i.e., those
with an orbital periods in the range of several months to few years. In the
framework of the GEE, the extra energy to sustain a high mass loss rate comes
from the accretion of mass from the giant envelope or its slow wind onto a more
compact secondary star. The secondary star energizes the outflow from the AGB
outer envelope by launching jets from the accretion disk.
