Elements of a sample model for which ﹩{e}_{{\rm{planet}}}=0.25﹩, ﹩\max {e}_{{\rm{p,free}}}=\max {i}_{{\rm{p,free}}}=0.02﹩ (in radians), and—for this figure alone—a fixed β = 0.4 for dust particles. Top row: inclination and eccentricity vector components of the planet (blue open circle), parent bodies (black points), and dust particles (red points). Forced eccentricities of parent bodies are shown as a red bar; full eccentricities differ from their forced values by up to ﹩\max {e}_{{\rm{p,free}}}﹩ (top right panel). Similarly, full inclinations differ from their forced values by up to ﹩\max {i}_{{\rm{p,free}}}﹩ (the half thickness of the disk). Because stellar radiation pressure does not alter orbital inclination, dust particle and parent body inclinations are identical (black points overlie red points in the top left panel). Bottom row: synthetic scattered light images for this disk seen face-on (alt = 90°, bottom left and middle panels) and seen 5° above the planet’s orbital plane (alt = 5°, az = 0°, bottom right panel). The scattered light features in the face-on (a.k.a. polar) view can be understood from an underlying “skeleton” of representative dust grain orbits, shown in matching colors in top and bottom middle panels. The nearly edge-on view in the right panel is such that the planet’s apoapse points toward the observer.