Zoomed-in images for ﹩{e}_{{\rm{planet}}}=0.25﹩ (top row) and ﹩{e}_{{\rm{planet}}}=0.7﹩ (bottom row). Left panels are nearly edge-on views (alt = 10°), and are each overlaid with a contour of constant surface brightness. Middle panels are face-on views showing representative dust grain orbits, color-coded to correspond to the colored points in the right-hand h–k plots (whose remaining symbols have meanings identical to those in Figure 1). Note how most particles in h–k space cluster near unit eccentricity as a consequence of our top-heavy β-distribution (13). The white dust orbit is launched from parent body periapse, and the green and yellow dust orbits are chosen to have median eccentricities and longitudes of periastron. As planet eccentricity increases, increasingly many dust orbits have their periastra aligned with that of the planet, leading to a more extended and sharply angled “fan” of emission in nearly edge-on views.