Mega-Planetary Rings

[stevebowers]

From that paper;

. It is therefore plausible that at an age when the protoplanetary disk around the primary star Gaia21bcv has largely dissipated, a smaller (only 1 au) disk at a substantial distance from the primary star, orbiting a secondary, less massive component, has escaped disk clearing and may still persist. While it appears clear that a massive body is needed to keep that occulting disk together, this object appears to be invisible and we cannot constrain its mass.
Anything from a low-mass star, a future brown dwarf, or a young giant planet would be possible.

A young giant planet surrounded by a 1AU accretion disk would be a spectacular sight, and this disk might eventually coalesce into a system of moons. I wonder how big the Hill sphere of such an object would be; even at 'a substantial distance from the star' I'd expect the 'less massive component' to be a superjovian world or brown dwarf, if it is not a protostar.