Planet formation in evolving protoplanetary discs
arXiv:1308.1791 · doi:10.1017/S1743921313008296
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.
10 pages, 4 figures. Invited review to appear in Proceedings of IAU Symposium 299, "Exploring the formation and evolution of planetary systems"
References in corpus (13)
- Protoplanetary Disk Structures in Ophiuchus
- Photoevaporation of protoplanetary discs II: evolutionary models and observable properties
- Photoevaporation of protoplanetary discs I: hydrodynamic models
- Pre-main-sequence isochrones -- II. Revising star and planet formation timescales
- On corotation torques, horseshoe drag and the possibility of sustained stalled or outward protoplanetary migration
- Line Emission from Gas in Optically Thick Dust Disks around Young Stars
- Formation and Evolution of Planetary Systems: Upper Limits to the Gas Mass in Disks Around Sun-like Stars
- Understanding the origin of the [OI] low-velocity component from T Tauri stars
- Deserts and pile-ups in the distribution of exoplanets due to photoevaporative disc clearing
- [NeII] emission line profiles from photoevaporative disc winds
- The Masses of Transition Circumstellar Disks: Observational Support for Photoevaporation Models
- From discs to planetesimals I: evolution of gas and dust discs
- Long-term Evolution of Photoevaporating Protoplanetary Disks