Disk Dispersal: Theoretical Understanding and Observational Constraints

Gorti, U. and Liseau, R. and Sándor, Z. and Clarke, C. (2015) Disk Dispersal: Theoretical Understanding and Observational Constraints. Space Science Reviews. ISSN 0038-6308 (Submitted)

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Abstract

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.

Item Type:	Article
Subjects:	Q Science / természettudomány > QB Astronomy, Astrophysics / csillagászat, asztrofizika
Depositing User:	Dr Zsolt Sándor
Date Deposited:	02 Oct 2015 13:37
Last Modified:	31 Dec 2016 00:15
URI:	http://real.mtak.hu/id/eprint/29446

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• Disk Dispersal: Theoretical Understanding and Observational Constraints. (deposited 02 Oct 2015 13:37) [Currently Displayed]
  • Disk Dispersal: Theoretical Understanding and Observational Constraints. (deposited 05 Oct 2016 14:10)

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