Cassini colleague Matt Hedman and other members of the imaging team have published a paper identifying an intriguing arc in Saturn’s G ring as the source of the particles in the rest of this faint dusty ring. Most dust rings in the solar system are associated with small moons. Enceladus’s geysers are responsible for most of the particles in the E ring. There are faint dust rings at Jupiter where the dust particles have orbits that clearly link them to individual moons. The moons produce the rings not through geologic activity like Enceladus, but as giant cosmic targets for interplanetary micrometeoroids which constantly pepper the moons at high speeds and knock off tiny bits of ice and rock. In the case of the G ring, Hedman found that there was a significantly brighter arc within the ring that is locked in a 7:6 corotation resonance with the moon Mimas. Apparently the particles in this G ring arc are knocking into each other and also being bombarded by meteoroids to act as a swarm of so-called “parent bodies” for the rest of the G ring (try calling your own parents that – it’s fun!), rather than an individual large satellite parent body. There’s even the chance that some of these mini-moonlets in the arc might be observed when Cassini flies particularly close to the G ring arc during Cassini’s extended mission, now in full-scale planning. I have a special interest in this study because I developed models of dust-ring production from swarms of parent bodies in the ring systems of Uranus and Neptune for my Ph.D. dissertation. The G ring appears to be similar, now, to the Adams ring of Neptune, the first ring known to have a distinct and long-lived arc, though the G ring is far fainter overall than the Adams ring.