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We use high resolution 3D hydrodynamical simulations to quantify the amountof 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, theconventional mass model ($M_1=120 M_{\odot}$ and $M_2=30 M_{\odot}$) and thehigh mass model ($M_1=170 M_{\odot}$ and $M_2=80 M_{\odot}$). The systemconsists of two very massive stars in a highly eccentric orbit. Every cycleclose to periastron passage the system experiences a spectroscopic event duringwhich many lines change their appearance, accompanied by a decline in x-rayemission associated with the destruction wind collision structure and accretionof the primary wind onto the secondary. We take four different numericalapproaches to simulate the response of the secondary wind to accretion. Eachaffects the mass loss rate of the secondary differently, and in turn determinesthe amount of accreted mass. The high mass model gives for most approaches muchmore accreted gas and a longer accretion phase. We find that the effectivetemperature of the secondary can be significantly reduced due to accretion. Wealso test different eccentricity values and a higher primary mass loss rate andfind their effect on the duration of the spectroscopic event. We conclude thatthe high mass model is better compatible with the amount of accreted mass,$\approx 3 \times 10^{-6} M_{\odot}$, required for explaining the reduction insecondary ionization photons during the spectroscopic event and compatible withits observed duration.

Simulating the Response of the Secondary Star of Eta Carinae to Mass Accretion at Periastron Passage