Toward Planetesimals in the Disk around TW Hydrae: 3.5 Centimeter Dust Emission

By D. Wilner, P. D’Alessio, N. Calvet, M. Claussen, L. Hartmann. 2005

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We present Very Large Array observations at λ = 3.5 cm of the nearby young star TW Hya that show the emission is constant in time over weeks, months, and years, and spatially resolved with peak brightness temperature ~10 K at ~0.″25 (15 AU) resolution. These features are naturally explained if the emission mechanism at this wavelength is thermal emission from dust particles in the disk surrounding the star. To account quantitatively for the observations, we construct a self-consistent accretion disk model that incorporates a population of centmeter-size particles that matches the long-wavelength spectrum and spatial distribution. A substantal mass fraction of orbiting particles in the TW Hya disk must have agglomerated to centmeter size. These data provide the first clear indication that dust emission from protoplanetary disks may be observed at centmeter wavelengths, and that changes in the spectral slope of the dust emission may be detected, providing constraints on dust evolution and the planet formation process.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/312b26a50ec77f27719d1836711aa0b514b6648b

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Citations in the corpus

Protoplanetary Disks and Their Evolution (2011, background): “The longest wavelength detection of dust in a protoplanetary disk to date was carried out by Wilner et al. (2005).”
Our astrochemical heritage (2012, background): “[122]; [468]; [416]; [464]; [12]; [223]; [112]; [274]; [262]), dust settling ([135]; [74]; [123]; [163]), dust processing (e.”
THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES (2011, methodology): “…(Krist et al. 2000; Trilling et al. 2001; Weinberger et al. 2002; Apai et al. 2004; Roberge et al. 2005), millimeter/radio-wave continuum images (Wilner et al. 2000, 2003, 2005; Hughes et al. 2007), and resolved molecular line maps (Qi et al. 2004, 2006, 2008; Hughes et al. 2008, 2011).”
High-Resolution Submillimeter Constraints on Circumstellar Disk Structure (2006, background): “…the auspices of more sophisticated models (e.g., D’Alessio et al. 2001; Calvet et al. 2002) to place ever more detailed constraints on properties like structure and chemistry (Wilner et al. 2003; Qi et al. 2003, 2004, 2006), as well as the signatures of grain growth (e.g., Wilner et al. 2005).”
RINGED SUBSTRUCTURE AND A GAP AT 1 au IN THE NEAREST PROTOPLANETARY DISK (2016, background): “Second, it is the benchmark case study for an evolved 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…”
Forming the cores of giant planets from the radial pebble flux in protoplanetary discs (2014, background): “…in cm wavelengths of the nearby young star TW Hya2 have revealed that as much as ∼10−3 M of the solid mass is present in cm-sized pebbles (Wilner et al. 2005), while 2 The age of TW Hya is estimated to be 5−10 Myr, but the star is possibly as young as ∼3 Myr based on near-infrared…”
Chemical enrichment of giant planets and discs due to pebble drift (2017, background): “Observations 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…”
Large dust particles in disks around T Tauri stars (2005, background): “There are, however, some observational indications that dust continuum emission may be a substantial source contributing to the centimetre fluxes of T Tauri stars (Rodriguez et al. 1994; Wilner et al. 1996, 2005).”
Theory of Star Formation (2007, background): “…with modeling to correct for optically-thick contributions varying with ν and R , with the resulting median β <∼ 1 (e.g. Natta et al. 2007; Andrews & Williams 2007; Lommen et al. 2007), suggesting that the largest “grains” are in fact cm-size pebbles (e.g. Wilner et al. 2005; Rodmann et al. 2006).”
Prograde rotation of protoplanets by accretion of pebbles in a gaseous environment (2009, background): “The inferred population of mm-cm pebbles can be very substantial, on the order of 10−3 solar masses (Wilner et al. 2005).”
CONSTRAINTS ON THE RADIAL VARIATION OF GRAIN GROWTH IN THE AS 209 CIRCUMSTELLAR DISK (2012, background): “Observations of dust in disks from sub-mm to cm wavelengths (Testi et al. 2001; Calvet et al. 2002; Testi et al. 2003; Natta & Testi 2004; Wilner et al. 2005; Rodmann et al. 2006; Lommen et al. 2009; Ricci et al. 2010a,b) have provided strong evidence for grain growth in disks.”
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).”
PARTICLE CLUMPING AND PLANETESIMAL FORMATION DEPEND STRONGLY ON METALLICITY (2009, background): “Coagulation-fragmentation mod- els (Brauer et al. 2008) and observations of pebbles in protoplanetary discs (Wilner et al. 2005) will be crucial for putting tighter constraints on the pebble abundance and the location of the metallicity switch.”
A Submillimeter View of Circumstellar Dust Disks in ρ Ophiuchi (2007, background): “Such growth is observationally reinforced by the remarkable centimeter-wave dust emission from large particles recently detected for the TW Hya disk (Wilner et al. 2005).”
Dust dynamics during protoplanetary disc clearing (2007, background): “…such holes remain uncertain, however, and previous studies have variously invoked the presence of a planet (e.g. Rice et al. 2003; Quillen et al. 2004), dust evolution (e.g. Wilner et al. 2005) or photoevaporation (e.g. Alexander et al. 2006b; Goto et al. 2006) to explain the observed " holes " .”