# Orbital Evolution of Moons in Weakly Accreting Circumplanetary Disks

## TL;DR

This paper models the formation and orbital evolution of moons in massive, hot circumplanetary disks, showing how migration can be halted and resonant systems formed due to disk structure changes.

## Contribution

It introduces a new evolutionary model for massive CPDs with weak MRI activity, explaining satellite migration stopping points and resonance formation.

## Key findings

- Inward migration can be halted by opacity transitions.
- Resonant satellite systems can form in these disks.
- Massive CPDs lead to diverse satellite orbital configurations.

## Abstract

We investigate the formation of hot and massive circumplanetary disks (CPDs) and the orbital evolution of satellites formed in these disks. Because of the comparatively small size-scale of the sub-disk, quick magnetic diffusion prevents the magnetorotational instability (MRI) from being well-developed at ionization levels that would allow MRI in the parent protoplanetary disk. In the absence of significant angular momentum transport, continuous mass supply from the parental protoplanetary disk leads to the formation of a massive CPD. We have developed an evolutionary model for this scenario and have estimated the orbital evolution of satellites within the disk. We find, in a certain temperature range, that inward migration of a satellite can be stopped by a change in the structure due to the opacity transitions. Moreover, by capturing second and third migrating satellites in mean motion resonances, a compact system in Laplace resonance can be formed in our disk models.