Protoplanetary Disks and Their Evolution

Flattened, rotating disks of cool dust and gas extending for tens to hundreds of astronomical units are found around almost all low-mass stars shortly after their birth. These disks generally persist for several million years, during which time some material accretes onto the star, some is lost thro...

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Bibliographic Details
Published in:Annual review of astronomy and astrophysics 2011-01, Vol.49 (1), p.67-117
Main Authors: Williams, Jonathan P, Cieza, Lucas A
Format: Article
Language:English
Subjects:
accretion
Astronomical instruments
Astrophysics
circumstellar matter
Disks
Evolutionary
Gases
Infrared radiation
Physical properties
Planet formation
pre-main sequence stars
Rotating disks
Solar system
Stars
Stars & galaxies
Wavelengths
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Summary:Flattened, rotating disks of cool dust and gas extending for tens to hundreds of astronomical units are found around almost all low-mass stars shortly after their birth. These disks generally persist for several million years, during which time some material accretes onto the star, some is lost through outflows and photoevaporation, and some condenses into centimeter- and larger-sized bodies or planetesimals. Through observations mainly at IR through millimeter wavelengths, we can determine how common disks are at different ages; measure basic properties including mass, size, structure, and composition; and follow their varied evolutionary pathways. In this way, we see the first steps toward exoplanet formation and learn about the origins of the Solar System. This review addresses observations of the outer parts, beyond 1 AU, of protoplanetary disks with a focus on recent IR and (sub)millimeter results and an eye to the promise of new facilities in the immediate future.
ISSN:0066-4146
1545-4282
DOI:10.1146/annurev-astro-081710-102548