The Dispersal of Protoplanetary Disks

Abstract

Protoplanetary disks are the sites of planet formation, and the evolution and eventual dispersal of these disks strongly influences the formation of planetary systems. Disk evolution during the planet-forming epoch is driven by accretion and mass-loss due to winds, and in typical environments photoevaporation by high-energy radiation from the central star is likely to dominate final gas disk dispersal. We present a critical review of current theoretical models, and discuss the observations that are used to test these models and inform our understanding of the underlying physics. We also discuss the role disk dispersal plays in shaping planetary systems, considering its influence on both the process(es) of planet formation and the architectures of planetary systems. We conclude by presenting a schematic picture of protoplanetary disk evolution and dispersal, and discussing prospects for future work.

23 pages, 6 figures. Refereed review chapter, accepted for publication in Protostars & Planets VI, University of Arizona Press (2014), eds. H.Beuther, C.Dullemond, Th.Henning, R.Klessen

Cited by in corpus (59)

• Fossilized condensation lines in the Solar System protoplanetary disk
• A stellar mass dependence of structured disks: a possible link with exoplanet demographics
• WASP-107b's density is even lower: a case study for the physics of planetary gas envelope accretion and orbital migration
• Impact splash chondrule formation during planetesimal recycling
• Bridging the gap between protoplanetary and debris disks: separate evolution of millimeter and micrometer-sized dust
• First versus second generation planet formation in post common envelope binary (PCEB) planetary systems
• Early Solar System instability triggered by dispersal of the gaseous disk
• The dispersal of protoplanetary discs. II: Photoevaporation models with observationally derived irradiating spectra
• Dispersal of protoplanetary disks by the combination of magnetically driven and photoevaporative winds
• The Dynamical Evolution of the Asteroid Belt
• Low EUV Luminosities Impinging on Protoplanetary Disks
• The determination of protoplanetary disk masses
• Signatures of an eccentric disc cavity: Dust and gas in IRS 48
• A dusty origin for the correlation between protoplanetary disc accretion rates and dust masses
• Transition disks: the observational revolution from SEDs to imaging
• Variable Accretion onto Protoplanet Host Star PDS 70
• Sub-Neptune Formation: The View from Resonant Planets
• Understanding the assembly of Kepler's compact planetary systems
• ALMA Survey of Lupus Class III Stars: Early Planetesimal Belt Formation and Rapid Disk Dispersal
• Formation of the polar debris disc around 99 Herculis
• Do the TRAPPIST-1 Planets Have Hydrogen-rich Atmospheres?
• Radiation-Hydrodynamical Models of X-ray Photoevaporation in Carbon Depleted Circumstellar Discs
• The influence of the environment on the spin evolution of low-mass stars. I. External photoevaporation of circumstellar disks
• Effects of photoevaporation on protoplanetary disc `isochrones'
• Binary-induced spiral arms inside the disc cavity of AB Aurigae
• TOI-216: Resonant Constraints on Planet Migration
• Stellar Oblateness versus Distant Giants in Exciting Kepler Planet Mutual Inclinations
• Which planets trigger longer-lived vortices: low-mass or high-mass?
• The Endgame of Gas Giant Formation: Accretion Luminosity and Contraction Post-Runaway
• Formation of Terrestrial Planets
• Impact of Cosmic-Ray Feedback on Accretion and Chemistry in Circumstellar Disks
• Multi-wavelength observations of protoplanetary discs as a proxy for the gas disc mass
• The importance of X-ray frequency in driving photoevaporative winds
• Unified simulations of planetary formation and atmospheric evolution II: Rapid disk clearing by photoevaporation yields low-mass super-Earth atmospheres
• Tidal Heating of Young Super-Earth Atmospheres
• A Secular Resonant Origin for the Loneliness of Hot Jupiters
• Migrating Low-Mass Planets in Inviscid Dusty Protoplanetary Discs
• High-resolution TNG spectra of T Tauri stars: Near-IR GIANO observations of the young variables XZ Tau and DR Tau
• Instabilities and Flow Structures in Protoplanetary Disks: Setting the Stage for Planetesimal Formation
• A brief overview of planet formation
• The general applicability of self-similar solutions for thermal disc winds
• Multiverse Predictions for Habitability: Number of Potentially Habitable Planets
• The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): VI. Comparison of Dust Evolution Models to AGE-PRO Observations
• Self-gravitating planetary envelopes and the core-nucleated instability
• Secular resonance sweeping and orbital excitation in decaying disks
• Modelling thermochemical processes in protoplanetary disks I: numerical methods
• Planet formation: key mechanisms and global models
• Dynamics of small grains in transitional discs
• Stellar Obliquity Excitation via Disk Dispersal-Driven Resonances in Binaries
• Planet Formation
• The effect of stellar evolution on dispersal of protoplanetary disks: Disk fraction in star-forming regions
• X-ray and UV radiation in the planet-forming T-Tauri system PDS 70. Signs of accretion and coronal activity
• Evidence of a Disk-wind Origin for Fluorescent H${}_2$ in Classical T Tauri Stars
• exoALMA XXI: The Morphology and Dynamics of Vertical Flows
• Dynamical Interactions in the Planetary System GJ4276
• The formation of planetary systems with SPICA
• A spatially-resolved large cavity of the J0337 protoplanetary disk in Perseus
• Searching for GEMS: Three warm Saturns and a super-Jupiter orbiting four early M-dwarfs
• History of the Solar Nebula from Meteorite Paleomagnetism