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In this paper, we present results from a multi-stage numerical campaign tobegin to explain and determine why extreme debris disk detections are rare,what types of impacts will result in extreme debris disks and what we can learnabout the parameters of the collision from the extreme debris disks. We beginby simulating many giant impacts using a smoothed particle hydrodynamical codewith tabulated equations of state and track the escaping vapour from thecollision. Using an $N$-body code, we simulate the spatial evolution of thevapour generated dust post-impact.  We show that impacts release vapour anisotropically not isotropically as hasbeen assumed previously and that the distribution of the resulting generateddust is dependent on the mass ratio and impact angle of the collision. Inaddition, we show that the anisotropic distribution of post-collision dust cancause the formation or lack of formation of the short-term variation in fluxdepending on the orientation of the collision with respect to the orbit aroundthe central star. Finally, our results suggest that there is a narrow region ofsemi-major axis where a vapour generated disk would be observable for anysignificant amount of time implying that giant impacts where most of theescaping mass is in vapour would not be observed often but this does not meanthat the collisions are not occurring.

Planetary Embryo Collisions and the Wiggly Nature of Extreme Debris Disks