Disk Inhomogeneities and the Origins of Planetary System Architectures and Observational Properties

TL;DR

This paper explores how structural inhomogeneities in protoplanetary disks influence planetary migration, creating traps that shape planetary system architectures and have observable signatures.

Contribution

It identifies multiple types of planet traps caused by disk inhomogeneities and analyzes their dependence on stellar and disk properties, advancing understanding of planetary system formation.

Findings

Disk inhomogeneities create planet traps that halt rapid migration.

Up to three trap types can coexist in a single disk.

Trap positions depend on stellar mass and disk accretion rate.

Abstract

Recent high-resolution observations show that protoplanetary disks have various kinds of structural properties or inhomogeneities. These are the consequence of a mixture of a number of physical and chemical processes taking place in the disks. Here, we discuss the results of our comprehensive investigations on how disk inhomogeneities affect planetary migration. We demonstrate that disk inhomogeneities give rise to planet traps - specific sites in protoplanetary disks at which rapid type I migration is halted. We show that up to three types of traps (heat transitions, ice lines and dead zones) can exist in a single disk, and that they move differently as the disk accretion rate decreases with time. We also demonstrate that the position of planet traps strongly depends on stellar masses and disk accretion rates. This indicates that host stars establish preferred (initial) scales of their planetary systems. Finally, we discuss the possible observational signatures of disk inhomogeneities.