CONSTRAINTS ON THE RADIAL VARIATION OF GRAIN GROWTH IN THE AS 209 CIRCUMSTELLAR DISK

By L. P'erez, J. Carpenter, C. Chandler, Andrea Isella, S. Andrews, L. Ricci, N. Calvet, S. Corder, A. Deller, C. Dullemond and 11 more. 2012

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We present dust continuum observations of the protoplanetary disk surrounding the pre-main-sequence star AS 209, spanning more than an order of magnitude in wavelength from 0.88 to 9.8 mm. The disk was observed with subarcsecond angular resolution (0.″2–0.″5) to investigate radial variations in its dust properties. At longer wavelengths, the disk emission structure is notably more compact, providing model-independent evidence for changes in the grain properties across the disk. We find that physical models which reproduce the disk emission require a radial dependence of the dust opacity κν. Assuming that the observed wavelength-dependent structure can be attributed to radial variations in the dust opacity spectral index (β), we find that β(R) increases from β < 0.5 at ∼20 AU to β > 1.5 for R ≳ 80 AU, inconsistent with a constant value of β across the disk (at the 10σ level). Furthermore, if radial variations of κν are caused by particle growth, we find that the maximum size of the particle-size distribution (amax) increases from submillimeter-sized grains in the outer disk (R ≳ 70 AU) to millimeter- and centimeter-sized grains in the inner disk regions (R ≲ 70 AU). We compare our observational constraint on amax(R) with predictions from physical models of dust evolution in protoplanetary disks. For the dust composition and particle-size distribution investigated here, our observational constraints on amax(R) are consistent with models where the maximum grain size is limited by radial drift.

Subfields: Astronomy and Astrophysics

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THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, background): “Moreover, recent multi-wavelength observations of disks suggest that optical depths remain low even for the high column densities expected at small disk radii, due to the natural decrease in particle emissivities produced by dust grain growth (e.g., Guilloteau et al. 2011; Pérez et al. 2012).”
Chemical enrichment of giant planets and discs due to pebble drift (2017, background): “…of protoplanetary discs show that there is a reservoir of such pebbles from which the embryos can accrete (Wilner et al. 2005; Rodmann et al. 2006; Lommen et al. 2007; Pérez et al. 2012; Tazzari et al. 2016), making pebble accretion an attractive model for the formation of giant planets.”
Gravitational Instabilities in Circumstellar Disks (2016, methodology): “Here again we rely on observations, which suggest a power law, or a power law plus exponential tail (Andrews et al. 2009; Pérez et al. 2012).”
FIRST RESULTS FROM HIGH ANGULAR RESOLUTION ALMA OBSERVATIO NS TOWARD THE HL TAU REGION (2015, background): “We do not find a gradual decrement of the spectral index with radius reported in other lower mass protoplanetary systems, albeit with reduced angular resolution (e.g. Guilloteau et al. 2011; Pérez et al. 2012).”
Evidence for the formation of comet 67P/Churyumov-Gerasimenko through gravitational collapse of a bound clump of pebbles (2017, background): “Very-long-wavelength observations show the pres- ence of mm-sized and larger grains in PPDs (see, e.g., van Boekel et al. 2004; D’Alessio et al. 2006; Natta et al. 2007; Birnstiel et al. 2010; Ricci et al. 2010; Pérez et al. 2012).”
DUST AND GAS IN THE DISK OF HL TAURI: SURFACE DENSITY, DUST SETTLING, AND DUST-TO-GAS RATIO (2015, background): “…that the larger grain abundances depend on radius, with a concentration toward the center of protoplanetary disks (Ricci et al. 2010; Guilloteau et al. 2011; Pérez et al. 2012; Menu et al. 2014); however, the spatial resolution was insufficient to resolve the vertical structure of the dust layer.”
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Dust Evolution and the Formation of Planetesimals (2016, background): “In recent years, the increasing resolution of (sub-)millimeter interferometers enabled radially resolved measurements of αmm, which can put constrains on the radial distribution of grain sizes (Isella et al. 2010; Guilloteau et al. 2011; Pérez et al. 2012; Trotta et al. 2013).”
One Solution to the Mass Budget Problem for Planet Formation: Optically Thick Disks with Dust Scattering (2019, background): “Previous spatially resolved α measurements have shown that α decreases towards the inner disk (Pérez et al. 2012, 2015; Tazzari et al. 2016; Carrasco-González et al. 2016).”
A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, background): “While Piétu et al. (2014) appear to have tentatively found a similar correlation at ∼230 GHz, we know empirically that the spatial extents of continuum emission from disks tend to increase with the observing frequency (e.g., Pérez et al. 2012, 2015; Menu et al. 2014; Tazzari et al. 2016).”
ALMA continuum observations of the protoplanetary disk AS 209. Evidence of multiple gaps opened by a single planet (2017, background): “Multi-frequency continuum observations revealed optically thin emission at millimeter wavelengths beyond a few 10 s of au from the star (Pérez et al. 2012; Tazzari et al. 2016).”
The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures (2018, background): “Multiwavelength observations are desirable for constraining dust optical depths (e.g., Pérez et al. 2012; Tazzari et al. 2016), but a rough estimate can still be obtained from the single-wavelength DSHARP observations by approximating the midplane temperature profile with the simplified expression…”
The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “Resolved variations in the continuum spectrum shape have been interpreted as radial gradients in the particle size distributions (larger solids closer to the star; Isella et al. 2010; Guilloteau et al. 2011; Pérez et al. 2012, 2015; Menu et al. 2014; Tazzari et al. 2016; Tripathi et al. 2018).”
Gas density drops inside dust cavities of transitional disks around young stars observed with ALMA (2015, background): “Also the size distribution of the dust is possibly not uniform throughout the disk: micron- and millimeter-sized grains may have different distributions (Garufi et al. 2013; van der Marel et al. 2013) and millimeter- and centimeter-sized grains can showradial variations (Pérez et al. 2012).”
Forming the cores of giant planets from the radial pebble flux in protoplanetary discs (2014, background): “Hints of a decrease in pebble size from cm in the inner disc to sub-mm in the outer disc (>∼75 AU) have also been seen in the protoplanetary disc of AS 209 (Pérez et al. 2012), CQ Tauri (Trotta et al. 2013) and TW Hydra (Menu et al. 2014).”