Short Version: The long-term fade may be produced by a stretched-out dust cloud in an outer orbit whereas the brief but deeper dips that have produced the most excitement are produced by small dust clouds in one or more inner orbits. The stretching-out of the outer orbit dust cloud is straightforward, since any expansion of particles (from a collision) would send some particles in slightly different orbits, with slightly different periods. If the periods have a range of 1%, for example, after 100 orbits the dust cloud would have a torus shape, and it would be capable of obstructing starlight continuously. As the torus circular cross-section expands (without changing orbit size), one edge of the torus would eventually enter our line-of-sight to the star. This is when we would observe the beginning of a gradually increasing fade. The torus may expand to completely obstruct the star, but when that happens it could be optically thin and produce only a small fade. Continued expansion could be accompanied by diminished loss of dust density along our line-of-sight, so expansion should eventually be associated with a recovery of star brightness. The “inverse Gaussian” model that I have employed for fitting the out-of-transit observations calls for a maximum fade amount of ~ 3 % in one or two years, followed by a slow recovery to normal star brightness in 5 or 10 years. During all of that time there will probably be short fades, lasting a few days, produced by dust clouds in orbits much closer to the star (but not closer than ~ 0.2 a.u.), with orbit periods of at least 4 weeks (but not less, due to the temperatures for closer orbits causing the particles to sublimate to gas).