Constraints on the Radial Variation of Grain Growth in the as 209 Circumstellar Disk

Pérez, Laura; Carpenter, John M.; Chandler, Claire J.; Isella, Andrea; Andrews, Sean M.; Ricci, Luca; Calvet, Nuria; Corder, Stuartt; Deller, Adam T.; Dullemond, C. P.; Greaves, J. S.; Harris, Robert J.; Henning, Thomas; Kwon, Woojin; Lazio, Joseph; Linz, H.; Mundy, Lee G.; Sargent, Anneila I.; Storm, Shaye; Testi, L.; Wilner, David J.

doi:10.1088/2041-8205/760/1/l17

Cited by 218 publications

(209 citation statements)

References 36 publications

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“…A significant conclusion is that the dust opacity spectral index varies with radius and decreases toward the center to values ≤1, indicating the presence of large grains (≥1 mm) in the inner regions of the disk (inside 100 AU). Our β(r) profiles agree with those found in other resolved disks (e.g., Guilloteau et al 2011;Pérez et al 2012Pérez et al , 2015Tazzari et al 2016).…”

Section: Discussionsupporting

confidence: 88%

“…The β(r) profiles are qualitatively consistent with the results of similar analyses performed in other classical smooth disks (Guilloteau et al 2011;Banzatti et al 2011;Pérez et al 2012Pérez et al , 2015Trotta et al 2013;Menu et al 2014;Tazzari et al 2016), with a significant variation of β throughout the disk (∆β > 1), indicating a maximum grain size a max decreasing with the distance from the star. The ALMA and VLA data provide for the first time the combination of signal-to-noise ratio, angular resolution and image fidelity to successfully perform an analysis in the image plane.…”

Section: β(R) Profiles and Grain Growthsupporting

confidence: 86%

“…With the high resolution of ALMA it is now possible to extend these studies and constrain the radial behavior of the opacity spectral index β (see, e.g., Pérez et al 2012Pérez et al , 2015, not just its average value across the disk. We recall here that the emission from the disk midplane is generally optically thin, and at these wavelengths the RayleighJeans regime is a good approximation.…”

Section: Spectral Index Profilesmentioning

confidence: 99%

“…These facilities allow us to obtain sensitive and high angular resolution observations of the dust continuum and gas emission lines from protoplanetary disks and therefore study the radial variations of the physical parameters of the disk. Recent results include the study of the dust properties as a function of radius in disks (e.g., Guilloteau et al 2011;Banzatti et al 2011;Pérez et al 2012Pérez et al , 2015Menu et al 2014;Tazzari et al 2016), and the clear identification of the CO snowline in nearby disks Qi et al 2013Qi et al , 2015, through its effects on DCO + and N 2 H + abundances. It is thus becoming possible to directly investigate the effect of the CO snowline on grain growth observationally.…”

Section: Introductionmentioning

confidence: 99%

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Dust properties across the CO snowline in the HD 163296 disk from ALMA and VLA observations

Guidi

Tazzari

Testi

et al. 2016

A&A

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Context. To characterize the mechanisms of planet formation it is crucial to investigate the properties and evolution of protoplanetary disks around young stars, where the initial conditions for the growth of planets are set. The high spatial resolution of Atacama Large Millimeter/submillimeter Array (ALMA) and Karl G. Jansky Very Large Array (VLA) observations now allows the study of radial variations of dust properties in nearby resolved disks and the investigation of the early stages of grain growth in disk midplanes. Aims. Our goal is to study grain growth in the well-studied disk of the young, intermediate-mass star HD 163296 where dust processing has already been observed and to look for evidence of growth by ice condensation across the CO snowline, which has already been identified in this disk with ALMA. Methods. Under the hypothesis of optically thin emission, we compare images at different wavelengths from ALMA and VLA to measure the opacity spectral index across the disk and thus the maximum grain size. We also use a Bayesian tool based on a two-layer disk model to fit the observations and constrain the dust surface density. Results. The measurements of the opacity spectral index indicate the presence of large grains and pebbles (≥1 cm) in the inner regions of the disk (inside ∼50 AU) and smaller grains, consistent with ISM sizes, in the outer disk (beyond 150 AU). Re-analyzing ALMA Band 7 science verification data, we find (radially) unresolved excess continuum emission centered near the location of the CO snowline at ∼90 AU. Conclusions. Our analysis suggests a grain size distribution consistent with an enhanced production of large grains at the CO snowline and consequent transport to the inner regions. Our results combined with the excess in infrared scattered light suggests there is a structure at 90 AU involving the whole vertical extent of the disk. This could be evidence of small scale processing of dust at the CO snowline.

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Section: Discussionsupporting

confidence: 88%

Section: β(R) Profiles and Grain Growthsupporting

confidence: 86%

Section: Spectral Index Profilesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Dust properties across the CO snowline in the HD 163296 disk from ALMA and VLA observations

Guidi

Tazzari

Testi

et al. 2016

A&A

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“…Therefore, the radial profile ofˇroughly corresponds to theǎ s a function of different grain sizes. There have been some observational constraints on the radial profile by using interferometric observations at radio wavelengths, which shows thatˇis small inside the disk and large outside the disk (e.g., Isella et al 2010;Guilloteau et al 2011;Pérez et al 2012Pérez et al , 2015Tazzari et al 2016). …”

Section: Opacity Evolutionmentioning

confidence: 99%

Dust Coagulation with Porosity Evolution

Kataoka

2017

Formation, Evolution, and Dynamics of Young Solar Systems

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Theoretical studies, laboratory experiments, and numerical simulations have shown several barriers in planetesimal formation, including radial drift, fragmentation, and bouncing problems. Also, observations of protoplanetary disks have shown the radial drift problems of millimeter-sized bodies at the outer orbital radius. The key to solving these problems is understanding porosity evolution. Dust grains become fluffy by coagulation in protoplanetary disks and this alters both the dynamic and optical properties of dust aggregates. First, we revealed the overall porosity evolution from micron-sized dust grains to kilometer-sized planetesimals; dust grains form extremely porous dust aggregates, where the filling factor is 10 4 , and then they are compressed by their collisions, the disk gas, and their self-gravity. In the coagulation process, they circumvent all the barriers if the monomers are 0.1-m icy bodies. The mass and porosity of the final product are consistent with those of the comets, which are believed to be the remnants of planetesimals. We further performed coagulation simulations including porosity evolution. We found that planetesimals can form inside 10 AU, avoiding the radial drift barrier. Furthermore, we calculated the opacity evolution of porous dust aggregates and found that the observed radio emission could be explained either by compact dust grains or by fluffy dust aggregates.

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Dust Evolution in Protoplanetary Disks

Andrews¹,

Birnstiel²

2018

Handbook of Exoplanets

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Over the past decade, advancement of observational capabilities, specifically the Atacama Large Millimeter/submillimeter Array (ALMA) and SPHERE instrument, alongside theoretical innovations like pebble accretion, have reshaped our understanding of planet formation and the physics of protoplanetary disks. Despite this progress, mysteries persist along the winded path of micrometer-sized dust, from the interstellar medium, through transport and growth in the protoplanetary disk, to becoming gravitationally bound bodies. This review outlines our current knowledge of dust evolution in circumstellar disks, yielding the following insights:• Theoretical and laboratory studies have accurately predicted the growth of dust particles to sizes that are susceptible to accumulation through transport processes like radial drift and settling. • Critical uncertainties in that process remain the level of turbulence, the threshold collision velocities at which dust growth stalls, and the evolution of dust porosity. • Symmetric and asymmetric substructure are widespread. Dust traps appear to be solving several long-standing issues in planet formation models, and they are observationally consistent with being sites of active planetesimal formation. • In some instances, planets have been identified as the causes behind substructures. This underlines the need to study earlier stages of disks to understand how planets can form so rapidly.In the future, better probes of the physical conditions in optically thick regions, including densities, turbulence strength, kinematics, and particle properties will be essential for unraveling the physical processes at play.

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Constraints on the Radial Variation of Grain Growth in the as 209 Circumstellar Disk

Cited by 218 publications

References 36 publications

Dust properties across the CO snowline in the HD 163296 disk from ALMA and VLA observations

Dust properties across the CO snowline in the HD 163296 disk from ALMA and VLA observations

Dust Coagulation with Porosity Evolution

Dust Evolution in Protoplanetary Disks

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