Angular momentum transport at a planet in the gaseous protoplanetary disk: a new version of an old model

Abstract

The evolution of the disk is influenced by both internal viscous torques and external torques brought on by one or more embedded planets. As planets form and grow within gaseous protoplanetary disks, the mutual gravitational interaction between the disk and planet leads to the exchange of angular momentum and migration of the planet. The functional depends on the tidal dissipation distribution in the disk which is concentrated in a vicinity ofthe protoplanets orbit. The aim of this work is to solve the equation for the evolution of the surface density of the disk according to the behavior of the angular momentum.

The evolution of the disk is influenced by both internal viscous torques and external torques brought on by one or more embedded planets. As planets form and grow within gaseous protoplanetary disks, the mutual gravitational interaction between the disk and planet leads to the exchange of angular momentum and migration of the planet. The functional depends on the tidal dissipation distribution in the disk which is concentrated in a vicinity ofthe protoplanets orbit. The aim of this work is to solve the equation for the evolution of the surface density of the disk according to the behavior of the angular momentum.