Model light curves for the tail morphology shown in Fig. 18 at wavelengths of 0.65 μm (solid blue), 0.85 μm (dashed orange) and 2.5 μm (dot-dashed red) compared with the Kepler long-cadence light curve of Kepler-1520 b (black). The model light curves are convolved to the Kepler long-cadence of 30 min. To simulate these light curves, the dust meta-particles were ejected with an initial radius of 50 μm. Due to 50 μm sized meta-particles not experiencing a significant radiation pressure, they do not form a long tail and drift in front of the planet. This results in a shallow transit depth and early ingress. To compensate for the reduced absorption resulting from the short tail, these light curves were scaled by a factor of 14 to make them comparable to the Kepler light curve.