Abstract
We discuss recent efforts to apply 3-D Smoothed Particle Hydrodynamics (SPH) simulations to model the binary wind collision in η Carinae, focusing on the Bore Hole effect, wherein the fast wind from the hot secondary star carves a cavity in the dense primary wind, allowing increased escape of radiation from the hotter/deeper layers of the primary's extended photosphere. This model may provide clues on how/where UV light is escaping the system, the illumination of distant material in various directions, and the parameters/orientation of the binary orbit. The role of interferometric observations in testing the models is also discussed.
