When we look at objects in the sky, out there in the solar system, galaxy and universe, we often see a pattern where numerous smaller or lighter items are scattered in a disk-shaped formation and are orbiting around something larger or heavier. For example, there are planetary rings, such as the prominent ones found around Saturn’s equator, which consist of things like dust, ice, rocks and moonlets. Then there is our Solar System: the Sun with the planets orbiting within a relatively flat disk around it — and the planets are thought to have formed from a protoplanetary disk. Also, at a larger scale we have, for example, the spiral galaxy with a central bulge and a rotating disk of stars around it (defining its galactic plane). So, rotating disks of celestial objects are quite common and repeated at every size scale; but how do they get to have that specific shape? Scientific explanations go along the lines of: the process starts with a cold cloud of gas and dust, the cloud collapses under gravity, and “conservation of angular momentum causes any small net rotation of the cloud to increase, forcing the material into a rotating disk”. But what does that really mean? Even astronomers say: “it’s so hard to explain in simple words”.