  We use high resolution 3D hydrodynamical simulations to quantify the amount
of mass accreted onto the secondary star of the binary system Eta Carinae,
exploring two sets of stellar masses that had been proposed for the system, the
conventional mass model ($M_1=120 M_{\odot}$ and $M_2=30 M_{\odot}$) and the
high mass model ($M_1=170 M_{\odot}$ and $M_2=80 M_{\odot}$). The system
consists of two very massive stars in a highly eccentric orbit. Every cycle
close to periastron passage the system experiences a spectroscopic event during
which many lines change their appearance, accompanied by a decline in x-ray
emission associated with the destruction wind collision structure and accretion
of the primary wind onto the secondary. We take four different numerical
approaches to simulate the response of the secondary wind to accretion. Each
affects the mass loss rate of the secondary differently, and in turn determines
the amount of accreted mass. The high mass model gives for most approaches much
more accreted gas and a longer accretion phase. We find that the effective
temperature of the secondary can be significantly reduced due to accretion. We
also test different eccentricity values and a higher primary mass loss rate and
find their effect on the duration of the spectroscopic event. We conclude that
the high mass model is better compatible with the amount of accreted mass,
$\approx 3 \times 10^{-6} M_{\odot}$, required for explaining the reduction in
secondary ionization photons during the spectroscopic event and compatible with
its observed duration.
