THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES

By S. Andrews, D. Wilner, A. Hughes, C. Qi, K. Rosenfeld, K. Oberg, T. Birnstiel, Catherine C. Espaillat, L. Cieza, Jonathan P. Williams and 2 more. 2011

210 citations recorded by the source corpus.

We present high-resolution (0.″3 = 16 AU), high signal-to-noise ratio Submillimeter Array observations of the 870 μm (345 GHz) continuum and CO J = 3 − 2 line emission from the protoplanetary disk around TW Hya. Using continuum and line radiative transfer calculations, these data and the multiwavelength spectral energy distribution are analyzed together in the context of simple two-dimensional parametric disk structure models. Under the assumptions of a radially invariant dust population and gas-to-dust mass ratio, we are unable to simultaneously reproduce the CO and dust observations with model structures that employ either a single, distinct outer boundary or a smooth (exponential) taper at large radii. Instead, we find that the distribution of millimeter-sized dust grains in the TW Hya disk has a relatively sharp edge near 60 AU, contrary to the CO emission (and optical/infrared scattered light) that extends to a much larger radius of at least 215 AU. We discuss some possible explanations for the observed radial distribution of millimeter-sized dust grains and the apparent CO-dust size discrepancy, and suggest that they may be hallmarks of substructure in the dust disk or natural signatures of the growth and radial drift of solids that might be expected for disks around older pre-main-sequence stars like TW Hya.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/bd032b8ae10f7d09ebc25341b7cddf527a5973c2

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Citations in the corpus

Forming the cores of giant planets from the radial pebble flux in protoplanetary discs (2014, background): “This radial power law profile is expected from the viscous evolution of an accretion disc (Lynden-Bell & Pringle 1974) and supported by the observed disc profile of the nearby protoplanetary disc around the star TW Hya (Andrews et al. 2012).”
Turbulence in the TW Hya Disk (2018, background): “Observations of the sub-mm dust continuum emission from around TW Hya (Weintraub et al. 1989; Hughes et al. 2009; Andrews et al. 2012; Qi et al. 2013; Hogerheijde et al. 2016; Nomura et al. 2016; Andrews et al. 2016) show variations of ∼10%, consistent with uncertainties in amplitude calibration.”
DUST FILTRATION BY PLANET-INDUCED GAP EDGES: IMPLICATIONS FOR TRANSITIONAL DISKS (2012, background): “Although submm observations (Andrews et al. 2012) have indeed suggested that the dust disk is more compact than the gaseous disk, the different surface density slopes between the dust and gas disks predicted in §5.4 need to be tested by future ALMA observations.”
RINGED SUBSTRUCTURE AND A GAP AT 1 au IN THE NEAREST PROTOPLANETARY DISK (2016, methodology): “…population of disk solids, with a radially concentrated population of larger (&cm) particles (Wilner et al. 2005; Menu et al. 2014) and a sharp radial decrease in the solids-to-gas mass ratio (Andrews et al. 2012; Birnstiel & Andrews 2014) that announce substantial growth and inward migration.”
Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, background): “In some cases, the central Gaussian profile is replaced with an exponentially tapered power law, which reproduces the oscillation pattern in the visibility profile (Andrews et al. 2012; Hogerheijde et al. 2016; Zhang et al. 2016) and better fits the data (with two more free parameters).”
A simple model for the evolution of the dust population in protoplanetary disks (2012, methodology): “The analytical profile has been scaled to fit the value of the dust profile from Andrews et al. (2012) at 10 AU.”
MAKE SUPER-EARTHS, NOT JUPITERS: ACCRETING NEBULAR GAS ONTO SOLID CORES AT 0.1 AU AND BEYOND (2014, methodology): “The protoplanetary disk TW Hydra is observed to have a dust-to-gas ratio that decreases radially outward (Andrews et al. 2012; see also Williams & Best 2014).”
Three Radial Gaps in the Disk of TW Hydrae Imaged with SPHERE (2016, methodology): “Nonetheless, the distribution of large dust could be resolved (Wilner et al. 2000; Hughes et al. 2007) and it was shown to be centrally concentrated with a sharp outer edge around 60 au using the SMA (Andrews et al. 2012).”
ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii (2018, methodology): “Small and bright optically thick cores are found in the ultra-high resolution ALMA observations of TW Hya (Andrews et al. 2016) and HL Tau (ALMA Partnership et al. 2015).”
Unveiling the gas-and-dust disk structure in HD 163296 using ALMA observations (2013, background): “A similar case of a dusty compact disk with a sharp outer edge smaller than the CO gaseous disk has been reported by Andrews et al. (2012) for TW Hya.”
Volatile carbon locking and release in protoplanetary disks. A study of TW Hya and HD 100546 (2016, background): “While mm-to-cm grains have been directly detected in the inner disk of TW Hya, the disk is strongly depleted of millimetre-sized grains outside of 60 au (Wilner et al. 2005; Andrews et al. 2012).”
WEAK TURBULENCE IN THE HD 163296 PROTOPLANETARY DISK REVEALED BY ALMA CO OBSERVATIONS (2015, methodology): “This model is based on the work of Rosenfeld et al. (2012, 2013), itself based on the structure laid out in Dartois et al. (2003), and has successfully been used to model CO emission from other disks (Andrews et al. 2012; Rosenfeld et al. 2012, 2013b, 2014; Williams & Best 2014).”
A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, methodology): “Surface Brightness Model Definition High quality observations of disk continuum emission have previously been modeled with “broken power-law” (e.g., Andrews et al. 2012; de Gregorio-Monsalvo et al. 2013; Hogerheijde et al. 2016) or “similarity solution” 0.1 1 % / arcsec 5 4 3 2 1 0 1 lo g I ν (%…”
On the diversity and statistical properties of protostellar discs (2018, background): “…the radius of the gas disc to be larger than that of the (sub-)mm dust disc (e.g. Piétu et al. 2007, 2014; Isella et al. 2007; Panić et al. 2009; Andrews et al. 2012; Rosenfeld et al. 2013; de Gregorio-Monsalvo et al. 2013; Walsh et al. 2014; Pineda et al. 2014; Cleeves et al. 2016; Barenfeld…”
A PARAMETRIC MODELING APPROACH TO MEASURING THE GAS MASSES OF CIRCUMSTELLAR DISKS (2013, background): “Note that these interpretations of low gas-to-dust ratios are a global disk average and are not inconsistent with the existence of locally high values in the outer disk due to inward migration of dust (Andrews et al. 2012).”
On planet formation in HL Tau (2015, result): “…et al. 2007; Kwon et al. 2011, 2015), these assume that the dust is co-located with the gas, whereas we expect settling and radial inward migration to produce a more compact dust disc, consistent with observations in other systems (Andrews et al. 2012; de Gregorio-Monsalvo et al. 2013).”
The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “…line emission have led to suggestions that the mass ratio of solids relative to gas also varies with radius (higher closer to the star; Panić et al. 2009; Andrews et al. 2012; de Gregorio-Monsalvo et al. 2013; Rosenfeld et al. 2013; Zhang et al. 2014; Facchini et al. 2017; Ansdell et al. 2018).”
A SPATIALLY RESOLVED VERTICAL TEMPERATURE GRADIENT IN THE HD 163296 DISK (2013, methodology): “Following the formalism explained by Andrews et al. (2012), axisymmetric density and temperature structures are defined using a polar cylindrical coordinate system (r, z).”