The Dispersal of Protoplanetary Disks

Alexander, R. D.; Pascucci, Ilaria; Andrews, Sean M.; Armitage, Philip J.; Cieza, Lucas A.

doi:10.2458/azu_uapress_9780816531240-ch021

Cited by 226 publications

(287 citation statements)

References 104 publications

(264 reference statements)

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270

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“…The fraction of accreting disks (withṀ acc > 10 −11 M ⊙ yr −1 ) in stellar groups declines on timescales similar to those of NIR excesses (Fedele et al 2010), with some non-accreting sources (withṀ acc < 10 −11 M ⊙ yr −1 ) still showing IR excesses (also Ingleby et al 2013, Hardy et al 2015. This may indicate that gas in the inner disk is removed first, consistent with dispersal scenarios (see Alexander et al 2014).…”

supporting

confidence: 59%

“…Overall, photoevaporation and viscous evolution together lead to the dispersal of gas on observed timescales (∼ 1 − 10 Myrs). For a more complete account of earlier work, we refer the reader to existing reviews of this topic (Hollenbach et al 2000, Dullemond et al 2007, Clarke 2011, Alexander et al 2014). …”

Section: Photoevaporation: Central Starmentioning

confidence: 99%

“…Other low velocity wind tracers such as [OI] forbidden line emission and CO rovibrational emission are more difficult to interpret with contributions from multiple components (Rigliaco et al 2013). For a more in-depth discussion, see Alexander et al (2014).…”

Section: Gas Diagnostics Of Photoevaporationmentioning

confidence: 99%

“…The main processes believed to disperse disks are a combination of viscous accretion and photoevaporation (see reviews by Hollenbach et al 2000, Armitage 2011, Clarke 2011, Alexander et al 2014 and to some extent, planet formation.…”

mentioning

confidence: 99%

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Disk Dispersal: Theoretical Understanding and Observational Constraints

et al. 2016

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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.

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supporting

confidence: 59%

Section: Photoevaporation: Central Starmentioning

confidence: 99%

Section: Gas Diagnostics Of Photoevaporationmentioning

confidence: 99%

mentioning

confidence: 99%

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Disk Dispersal: Theoretical Understanding and Observational Constraints

et al. 2016

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“…Even if CO-poor gas extended down to 0.1 au, with the same surface density profile as inferred from the outer disk, accretion would still be able to deplete the disk in ∼5000 years. A photoevaporative flow can also remove gas from the disk on similar timescales (Alexander et al 2014, and references therein). The CO itself can be selectively removed through its photodissociation by high energy photons.…”

Section: Discussionmentioning

confidence: 99%

Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

Flaherty

Hughes

Andrews

et al. 2016

ApJ

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The disk around HD 141569 is one of a handful of systems whose weak infrared emission is consistent with a debris disk, but still has a significant reservoir of gas. Here we report spatially resolved millimeter observations of the CO(3-2) and CO(1-0) emission as seen with the Submillimeter Array and CARMA. We find that the excitation temperature for CO is lower than expected from cospatial blackbody grains, similar to previous observations of analogous systems, and derive a gas mass that lies between that of gas-rich primordial disks and gas-poor debris disks. The data also indicate a large inner hole in the CO gas distribution and an outer radius that lies interior to the outer scattered light rings. This spatial distribution, with the dust rings just outside the gaseous disk, is consistent with the expected interactions between gas and dust in an optically thin disk. This indicates that gas can have a significant effect on the location of the dust within debris disks.

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Challenges in planet formation

2016

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Over the past two decades, large strides have been made in the field of planet formation. Yet fundamental questions remain. Here we review our state of understanding of five fundamental bottlenecks in planet formation. These are the following: (1) the structure and evolution of protoplanetary disks; (2) the growth of the first planetesimals; (3) orbital migration driven by interactions between protoplanets and gaseous disk; (4) the origin of the Solar System's orbital architecture; and (5) the relationship between observed super‐Earths and our own terrestrial planets. Given our lack of understanding of these issues, even the most successful formation models remain on shaky ground.

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The Dispersal of Protoplanetary Disks

Cited by 226 publications

References 104 publications

Disk Dispersal: Theoretical Understanding and Observational Constraints

Disk Dispersal: Theoretical Understanding and Observational Constraints

Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

Challenges in planet formation

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