Anubis exhibits rings, like most of the gaseous planets in our solar system. The rings are optically thin, which means that very little material is present and most of the light passes through. The faint and almost undetectable rings have a small optical depth, which measures the transparency of the ring system. The rings contain bends, kinks, and clumps that give the illusion that the strands are braided.

They are composed mainly of ice and traces of carbon minerals and dust. The radial distance from the core of Anubis was observed to be 175,600 km to the ansa, which is the portion of the ring that is the farthest from the planet. This would lead us to believe that there are satellites or moons as yet to be discovered. Because we know that there must be sheppard satellites in order to have rings.

Rings are held together from the particles pulling themselves together via their own gravity, while the planet tries to tug the ring inward. At the same time, the satellites pull the particles outward. The combination of the planet and the satellite tugging on the particle keep the rings in orbit with the planet.

The distance which separates the regions where rings exist from the region where satellites form is called the Roche Limit. The Roche Limit is defined by

r/R = 2(p/ps)1/3

where p is the density and R is the radius of the planet; ps is the density and r is the radius of the satellite. When the two densities are equal, the equation becomes

r = 2.44R

For Anubis, if the planet and the satellite have the same densities, the Roche Limit would be 175,680 km, which leads us to believe that there is a satellite with the same density out there somewhere. And that the ring is less than 80 km wide since rings are always found inside the Roche Limit.