Disk Dispersal: Theoretical Understanding and Observational Constraints
Artikel i vetenskaplig tidskrift, 2016

Protoplanetary disks dissipate rapidly after the central star forms, on time-scales comparable to those inferred for planet formation. In order to allow the formation of planets, disks must survive the dispersive effects of UV and X-ray photoevaporation for at least a few Myr. Viscous accretion depletes significant amounts of the mass in gas and solids, while photoevaporative flows driven by internal and external irradiation remove most of the gas. A reasonably large fraction of the mass in solids and some gas get incorporated into planets. Here, we review our current understanding of disk evolution and dispersal, and discuss how these might affect planet formation. We also discuss existing observational constraints on dispersal mechanisms and future directions.

Winds

Planet formation

Accretion

Protoplanetary disks

Författare

U. Gorti

NASA Ames Research Center

René Liseau

Chalmers, Rymd- och geovetenskap, Radioastronomi och astrofysik

Z. Sándor

Magyar Tudomanyos Akademia

C. Clarke

University of Cambridge Institute of Astronomy

Space Science Reviews

0038-6308 (ISSN) 1572-9672 (eISSN)

Vol. 205 1-4 125-152

Ämneskategorier

Astronomi, astrofysik och kosmologi

Infrastruktur

Onsala rymdobservatorium

DOI

10.1007/s11214-015-0228-x

Mer information

Senast uppdaterat

2018-07-04