PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS

By S. Andrews, D. Wilner, A. Hughes, C. Qi, C. Dullemond. 2009

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We present the results of a high angular resolution (0.″3 ≈ 40 AU) Submillimeter Array survey of the 345 GHz (870 μm) thermal continuum emission from nine of the brightest, and therefore most massive, circumstellar disks in the ∼1 Myr-old Ophiuchus star-forming region. Using two-dimensional radiative transfer calculations, we simultaneously fit the observed continuum visibilities and broadband spectral energy distribution for each disk with a parametric structure model. Compared to previous millimeter studies, this survey includes significant upgrades in modeling, data quality, and angular resolution that provide improved constraints on key structure parameters, particularly those that characterize the spatial distribution of mass in the disks. In the context of a surface density profile motivated by similarity solutions for viscous accretion disks, Σ ∝ (R/Rc)−γexp [ − (R/Rc)2−γ], the best-fit models for the sample disks have characteristic radii Rc ≈ 20–200 AU, high disk masses Md ≈ 0.005–0.14 M☉ (a sample selection bias), and a narrow range of radial Σ gradients (γ ≈ 0.4–1.0) around a median γ = 0.9. These density structures are used in conjunction with accretion rate estimates from the literature to help characterize the viscous evolution of the disk material. Using the standard prescription for disk viscosities, those combined constraints indicate that α ≈ 0.0005–0.08. Three of the sample disks show large (R ≈ 20–40 AU) central cavities in their continuum emission morphologies, marking extensive zones where dust has been physically removed and/or has significantly diminished opacities. Based on the current requirements of planet formation models, these emission cavities and the structure constraints for the sample as a whole suggest that these young disks may eventually produce planetary systems, and have perhaps already started.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/a697b7c51c51f1ecf79de4a60e064bfbb80ab5ba

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Citations in the corpus

REVEALING A UNIVERSAL PLANET–METALLICITY CORRELATION FOR PLANETS OF DIFFERENT SIZES AROUND SOLAR-TYPE STARS (2013, background): “…circumstellar disk clears before the outer regions (e.g., Isella et al. 2009), and imaging surveys of the brightest disks in the nearby Ophiuchus star forming region demonstrate that central clearings are very common in even the most massive disks at ages of a few Myr (Andrews et al. 2009, 2010).”
The Disk Substructures at High Angular Resolution Project (DSHARP). VI. Dust Trapping in Thin-ringed Protoplanetary Disks (2018, background): “From an observational perspective, the radial drift problem manifests itself by the presence of large grains in the outer regions of protoplanetary disks (Testi et al. 2003; Andrews et al. 2009; Ricci et al. 2010), which appears to be in conflict with theoretical predictions (Brauer et al. 2007).”
DUST AND GAS IN THE DISK OF HL TAURI: SURFACE DENSITY, DUST SETTLING, AND DUST-TO-GAS RATIO (2015, methodology): “We use standard disk parameters to describe the disk structure (e.g. Pinte et al. 2008a; Andrews et al. 2009, see Section 3.1) except for the surface density which shape is let free and is fitted for.”
Global Simulations of the Inner Regions of Protoplanetary Disks with Comprehensive Disk Microphysics (2017, methodology): “…that these instabilities all require certain thermodynamic conditions to operate, the resulting level of turbulence is typically weak, with Shakura–Sunyaev α reaching ∼10−3 at most, which is too small to account for the accretion rates in the bulk disk population (e.g., Andrews et al. 2009, 2010).”
WIND-DRIVEN ACCRETION IN PROTOPLANETARY DISKS. I. SUPPRESSION OF THE MAGNETOROTATIONAL INSTABILITY AND LAUNCHING OF THE MAGNETOCENTRIFUGAL WIND (2013, background): “The surface density of the inner PPDs is highly uncertain and have not been well constrained observationally (the situation is better for the outer disk with millimeter interferometric observations, e.g., Andrews et al. 2009).”
Our astrochemical heritage (2012, background): “presence of crystalline silicates; [244]; [314]; [389]; [297]; [330]; [373]), inner holes (probably carved by a planet or by photoevaporation, [75]; [215]; [14]; [13]; [106]).”
Protoplanetary Disks and Their Evolution (2011, methodology): “• There is a wide range of transition disk SEDs, indicative of the varied physical processes, photoevaporation, grain growth, and dynamical interactions with companions or planets, that produce them.”
DUST FILTRATION BY PLANET-INDUCED GAP EDGES: IMPLICATIONS FOR TRANSITIONAL DISKS (2012, result): “…1992; Calvet et al. 2002, 2005; Rice et al. 2003; Schneider et al. 2003; Espaillat et al. 2007, 2008, 2010; Hughes et al. 2009), an interpretation confirmed in some cases via direct sub-mm imaging (e.g., Pietu et al. 2006; Brown et al. 2007, 2009; Hughes et al. 2009; Andrews et al. 2009, 2011).”
The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “′′3) resolution for selection (Andrews et al. 2009, 2010; Ansdell et al. 2016; Barenfeld et al. 2016).”
Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, methodology): “…the model of the protoplanetary disk is on one hand the observational progress that has been made in the last few years also in this field (e.g. Andrews et al. 2009, 2010; Fedele et al. 2010), but also the theoretical result that the disk structure is very important for the final properties of…”
The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures (2018, methodology): “We classify them as annular substructures because they still appear to represent deviations from standard “smooth” disk profiles (e.g., Andrews et al. 2009; Tazzari et al. 2017).”
ALMA continuum observations of the protoplanetary disk AS 209. Evidence of multiple gaps opened by a single planet (2017, unknown): “(†) Andrews et al. (2009).”
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, methodology): “This demonstration followed the general modeling formalism outlined by Andrews et al. (2009, 2011).”