Prototypical debris disk morphologies seen in scattered light, as captured by a “minimum model” (single eccentric planet + ring of parent bodies + dust grains + stellar radiation pressure). Possible observable shapes include a “ring” (top left), a “needle” (middle left; this is essentially a ring seen edge-on), and a “ship-and-wake” (bottom left; this is basically a needle which is fat enough to resolve vertical structure). Right panels feature various kinds of “moths,” either our standard version where most dust grains are in front of the star and therefore appear bright in forward-scattered light (top right), a moth with “double wings” where dust grain orbits are perfectly apsidally aligned as a consequence of assuming that grains are launched exclusively from parent body periastra (middle right), and a “reverse moth” where most grains are behind the star, accompanied by a “bar” in front of the star (bottom right). Note the sharp wingtips seen in the “double wing” panel; this model looks encouragingly similar to HD 32297 (Schneider et al. 2014, their Figure 19b). The surface brightness contrasts between the brightest and the faintest features are ∼36, ∼900, ∼10⁴, ∼260, ∼620, and ∼400 for the ring, needle, ship-and-wake, moth, double wing, and bar, respectively. The head of the ship is ∼400× brighter than its stern. In the double wing, the two wings are ∼4× brighter than the gap between them. The bar is ∼20% brighter than the gap that separates it from the main disk.