A dual-frequency sub-arcsecond study of proto-planetary disks at mm wavelengths: first evidence for radial variations of the dust properties

By S. Guilloteau, A. Dutrey, V. Pi'etu, Y. Boehler. 2011

208 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/7c1930a1965523977ac5f433a9d56602a86a61f2

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In Astronomy and Astrophysics

Citations in the corpus

Multiwavelength analysis for interferometric (sub-)mm observations of protoplanetary disks - Radial constraints on the dust properties and the disk structure (2015, methodology): “The amax(R) radial profiles derived for the three disks tend towards similar values amax(R) ' 2 cm in the innermost spatially resolved region 10 AU R 20 AU, but display apparent differences in the slope with AS 209, FT Tau, and DR Tau showing respectively an increasing steepness.”
A STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATION (2016, background): “Previous work has pointed out that dust disk radii correlate positively with millimeter fluxes for TTauri stars (Isella et al. 2009; Andrews et al. 2010; Guilloteau et al. 2011), but the scatter is large and what is really needed is to demonstrate a correlation with stellar mass.”
A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, background): “…albeit in that case for the peripherally related quantities of disk mass and “characteristic” size.6 Piétu et al. (2014) also claimed a size– luminosity trend in their analogous 230 GHz (1.3 mm) sample (∼25 disks, including data from Guilloteau et al. 2011), although they did not quantify it.”
Gaps, Rings, and Non-Axisymmetric Structures in Protoplanetary Disks - From Simulations to ALMA Observations (2014, unknown): “Rodriguez et al. 2010; Schegerer et al. 2006), 100 pc (e.g., CQ Tau, Guilloteau et al. 2011), 120 pc (e.g., Oph IRS 48, van der Marel et al. 2013), and 140 pc (e.g., HD 169142, Honda et al. 2012).”
MILLIMETER-WAVE POLARIZATION OF PROTOPLANETARY DISKS DUE TO DUST SCATTERING (2015, background): “…β ≈ 0 − 1, where κdust ∝ λ−β (e.g., Beckwith & Sargent 1991; Wilner et al. 2000; Kitamura et al. 2002; Andrews & Williams 2005; Ricci et al. 2010b,a; Guilloteau et al. 2011), which suggests that dust grains are grown to millimeter in size (e.g., Miyake & Nakagawa 1993; D’Alessio et al.…”
ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii (2018, background): “…assuming transition disks had the same grain population as full disks before the inner disk clearing, and also that βd increases with radius (e.g., Guilloteau et al. 2011; Tazzari et al. 2016), then disks with large inner cavities should lack large grains and therefore appear to have higher αmm…”
The Disk Substructures at High Angular Resolution Project (DSHARP). V. Interpreting ALMA Maps of Protoplanetary Disks in Terms of a Dust Model (2018, methodology): “With high angular resolution observations this can now be done as a function of radial coordinate in the disk (e.g., Guilloteau et al. 2011; Isella et al. 2010; Pérez et al. 2012), and shows that bright rings have shallower slopes than the dark annuli between them (e.g. ALMA Partnership et al.…”
Observational Signatures of Planets in Protoplanetary Disks I: Gaps Opened by Single and Multiple Young Planets in Disks (2014, background): “…in Millimeter-wave Astronomy (e.g. Isella et al. 2009, 2010; Ricci et al. 2013), the Plateau de Bure Interferometer (e.g. Piétu et al. 2006; Guilloteau et al. 2011), and the newly commissioned Atacama Large Millimeter Array (ALMA) (e.g. van der Marel et al. 2013; Casassus et al. 2013;…”
Ring shaped dust accumulation in transition disks (2012, background): “The same physical process happens to the millimeter-size particles that are observed in the outer regions of the disk (e.g., Wilner et al. 2000; Ricci et al. 2010; Guilloteau et al. 2011).”
Chemical enrichment of giant planets and discs due to pebble drift (2017, background): “The numerous discs in which the dust radii are observed to be smaller than their gas radii (Guilloteau et al. 2011; Andrews et al. 2012; Piétu et al. 2014; Birnstiel & Andrews 2014) provide evidence for on going radial drift.”
Trapping dust particles in the outer regions of protoplanetary disks (2011, background): “…Andrews & Williams (2005); Rodmann et al. (2006); Natta et al. (2007); Isella et al. (2009); Lommen et al. (2009); Ricci et al. (2010a, 2011); Guilloteau et al. (2011)) that suggests a mechanism operating that prevents the rapid inward drift (Klahr & Henning (1997), Brauer et al. (2007),…”
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).”
DUST AND GAS IN THE DISK OF HL TAURI: SURFACE DENSITY, DUST SETTLING, AND DUST-TO-GAS RATIO (2015, background): “…now suggesting 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…”
CONSTRAINTS ON THE RADIAL VARIATION OF GRAIN GROWTH IN THE AS 209 CIRCUMSTELLAR DISK (2012, methodology): “Observations of disks in Taurus at 1.3 and 3 mm with CARMA15 (Isella et al. 2010) and PdBI16 15 Combined Array for Research in Millimeter-wave Astronomy (Guilloteau et al. 2011), have constrained β as a function of radius.”
THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES (2011, background): “Some recent studies have made progress in extracting the radial (surface) density profiles in these disks from high angular resolution measurements of their millimeterwave continuum emission (Andrews et al. 2009, 2010b; Isella et al. 2009; Guilloteau et al. 2011).”
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).”
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).”