Protoplanetary Disks and Their Evolution

Details Protoplanetary Disks and Their Evolution Protoplanetary Disks and Their Evolution

2011-03-02

arxiv.org/abs/1103.0556v2

2011, Ann. Rev. Astr. Astrophys., 49, 67

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

65 pages, 11 figures, published in volume 49 of the Annual Review of Astronomy and Astrophysics, based on the available litera

Scientific paper

10.1146/annurev-astro-081710-102

Flattened, rotating disks of cool dust and gas extending for tens to hundreds of AU are found around almost all low mass stars shortly after their birth. These disks generally persist for several Myr, 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 infrared 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 infrared and (sub-)millimeter results and an eye to the promise of new facilities in the immediate future.

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