PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS. II. EXTENSION TO FAINTER SOURCES

By S. Andrews, D. Wilner, A. Hughes, C. Qi, C. Dullemond. 2010

300 citations recorded by the source corpus.

We present new results from a significant extension of our previous high angular resolution (0.″3 ≈ 40 AU) submillimeter array survey of the 340 GHz (880 μm) thermal continuum emission from dusty circumstellar disks in the ∼1 Myr old Ophiuchus star-forming region. An expanded sample is constructed to probe disk structures that emit significantly lower millimeter luminosities (hence dust masses), down to the median value for T Tauri stars. Using a Monte Carlo radiative transfer code, the millimeter visibilities and broadband spectral energy distribution for each disk are simultaneously reproduced with a two-dimensional parametric model for a viscous accretion disk that has a surface density profile Σ ∝ (R/Rc)−γexp [ − (R/Rc)2−γ]. We find wide ranges of characteristic radii (Rc = 14–198 AU) and disk masses (Md = 0.004–0.143 M☉), but a narrow distribution of surface density gradients (γ = 0.4–1.1) that is consistent with a uniform value 〈γ〉 = 0.9 ± 0.2 and independent of mass (or millimeter luminosity). In this sample, we find a correlation between the disk luminosity/mass and characteristic radius, such that fainter disks are both smaller and less massive. We suggest that this relationship is an imprint of the initial conditions inherited by the disks at their formation epoch, compare their angular momenta with those of molecular cloud cores, and speculate on how future observations can help constrain the distribution of viscous evolution timescales. No other correlations between disk and star properties are found. The inferred disk structures are briefly compared with theoretical models for giant planet formation, although resolution limitations do not permit us to directly comment on material inside R ≈ 20 AU. However, there is some compelling evidence for the evolution of dust in the planet formation region: 4/17 disks in the sample show resolved regions of significantly reduced millimeter optical depths within ∼20–40 AU of their central stars.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/75e2696e7726977b25b820bed9ebd176be16f5a3

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Citations in the corpus

Possible planet-forming regions on submillimetre images (2011, background): “Note that there exist further examples of discs showing non-axisymmetric submillimetre images, such as LkCa 15 (Piétu et al. 2006), GM Aur (Hughes et al. 2009), SR 24S (Andrews et al. 2010), and J1604-2130 (Williams & Cieza 2011) for which the same phenomenon might be responsible.”
Protoplanetary disc evolution and dispersal: the implications of X-ray photoevaporation (2010, background): “Such a choice is appealing both observationally and theoretically, since it predicts a surface density scaling as Σ ∝ R−1 which is supported by observations (e.g. Hartmann et al 1998; Andrews et al. 2010) and is consistent with a constant α disc which is mildly flaring i.e.”
Observational Signatures of Planets in Protoplanetary Disks I: Gaps Opened by Single and Multiple Young Planets in Disks (2014, methodology): “…continuum and/or molecular line emission have been carried out for a few dozens nearby disks using the Submillimeter Array (e.g. Brown et al. 2009; Andrews et al. 2009, 2010, 2011), the Combined Array for Research in Millimeter-wave Astronomy (e.g. Isella et al. 2009, 2010; Ricci et al. 2013),…”
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).”
One Solution to the Mass Budget Problem for Planet Formation: Optically Thick Disks with Dust Scattering (2019, methodology): “Dust Disk Size - Luminosity Relationship Recent surveys (Tripathi et al. 2017; Andrews et al. 2018a) confirm the previous hinted linear relationship (Andrews et al. 2010) between the submm continuum luminosity and its emitting surface area.”
RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, background): “Aside from the large dust-depleted cavities, these transition disks have surface density profiles similar to those inferred for normal disks (see Andrews et al. 2009, 2010b).”
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…”
On the diversity and statistical properties of protostellar discs (2018, methodology): “In Lupus, Tazzari et al. (2017) give the number of systems that they are unable to determine disc radii for, but there is no indication of completeness in the studies of Andrews et al. (2009, 2010) and Tripathi et al. (2017).”
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.”
On the theory of disc photoevaporation (2011, methodology): “Power-law variation of mid-plane variables is an expectation of the Lynden-Bell & Pringle (1974) similarity solutions and appears to be consistent with observational estimates of disc surface density profiles which suggest that ∝ R−1 (Andrews et al. 2010).”
Debris disks as signposts of terrestrial planet formation (2011, background): “In addition, recent observations suggest that low-mass disks are more compact (Andrews et al. 2010) so there may be a correlation between the disk mass and the location of planet formation as well (see also Kennedy & Kenyon 2008).”
Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, background): “Observations of disks around young stars have provided us with knowledge of the distributions of disk masses (Beckwith & Sargent 1996; Andrews et al. 2009), disk sizes (McCaughrean & Odell 1996; Andrews et al. 2010) and lifetimes (Haisch et al. 2001; Fedele et al. 2010).”
Trapping dust particles in the outer regions of protoplanetary disks (2011, background): “…= Σ0 ( r rc )−γ exp − ( rrc )2−γ , (2) where rc is the characteristic radius, taken to be 60AU, and γ is the viscosity power index equal to 1, which are the median values found from high angular resolution imaging in the sub-mm of disks in the Ophiucus star forming regions (Andrews et al. 2010).”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, methodology): “Motivated by observations (Andrews et al., 2009, 2010) and viscous disk theory (Lynden-Bell and Pringle, 1974; Chambers, 2006; Bitsch et al., 2015) we chose a simple power-law profile for the disk.”
Planetesimal formation starts at the snow line (2017, background): “Observational constraints place the outer edge of the disk anywhere between 60 AU and several hundreds AU (Andrews et al. 2009, 2010).”
A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, methodology): “As α increases, the profiles converge to a sharp broken power-law. surface brightness profiles (e.g., Andrews et al. 2009, 2010; Isella et al. 2009, 2010).”
TRANSITIONAL DISKS AS SIGNPOSTS OF YOUNG, MULTIPLANET SYSTEMS (2011, methodology): “Some disks for which small, 3- 4 AU inner holes were inferred based on SED modeling— including the canonical transitional disk, GM Aur—were shown to have large inner clearings of 15 AU or more once imaged at high angular resolution (Hughes et al. 2009; Andrews et al. 2010, 2011).”
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.”
CONSTRAINTS ON THE RADIAL VARIATION OF GRAIN GROWTH IN THE AS 209 CIRCUMSTELLAR DISK (2012, background): “Resolved 0.88 mm continuum observations reveal a smooth radial density structure down to 0.3′′ ∼ 40 AU (Andrews et al. 2009, 2010).”