  We apply the previously suggested accretion model for the behavior of the
super-massive binary system Eta Carinae close to periastron passages. In that
model it is assumed that for ~10 weeks near periastron passages one star is
accreting mass from the slow dense wind blown by the other star. We find that
the secondary, the less massive star, accretes ~2x10^{-6}Mo. This mass
possesses enough angular momentum to form a disk, or a belt, around the
secondary. The viscous time is too long for the establishment of equilibrium,
and the belt must be dissipated as its mass is being blown in the reestablished
secondary wind. This processes requires about half a year, which we identify
with the recovery phase of Eta Carinae. We show that radiation pressure, termed
radiative braking, cannot prevent accretion. In addition to using the commonly
assumed binary model for Eta Carinae, we also examine alternative models where
the stellar masses are larger, and/or the less massive secondary blows the slow
dense wind, while the primary blows the tenuous fast wind and accretes mass for
~10 weeks near periastron passages. We end by some predictions for the next
event (January-March 2009).
