Planet formation in evolving protoplanetary discs

TL;DR

This paper reviews the physics of evolving protoplanetary discs, focusing on how accretion and photoevaporation influence disc evolution, and discusses how observations inform our understanding of planet formation and migration.

Contribution

It provides a comprehensive summary of disc evolution processes and their impact on planet formation, integrating observational data with theoretical models.

Findings

Disc evolution is primarily driven by accretion and photoevaporation.

Observations are crucial for testing disc evolution models.

Understanding disc evolution informs planet formation and migration theories.

Abstract

I attempt to summarize our knowledge of planet formation in evolving protoplanetary discs. I first review the physics of disc evolution and dispersal. For most of the disc lifetime evolution is driven by accretion and photoevaporation, and I discuss how the interplay between these processes shapes protoplanetary discs. I also discuss the observations that we use to test these models, and the major uncertainties that remain. I will then move on to consider planet formation and migration in evolving discs, and discuss how observations of both discs and planets can be used to inform our understanding of protoplanetary disc evolution.