Large grains in the disk of CQ Tau

By L. Testi, A. Natta, D. Shepherd, D. Wilner. 2003

172 citations recorded by the source corpus.

We present 7 mm observations of the dusty disk surrounding the 10 Myr old 1.5 Mpre-main-sequence star CQ Tauri obtained at the Very Large Array with 0.8 arcsec resolution and 0.1 mJy rms sensitivity. These observations resolve the 7 mm emission in approximately the north-south direction, confirming previous results obtained with lower resolution. We use a two- layer flared disk model to interpret the observed fluxes from 7 mm to 1.3 mm together with the resolved 7 mm structure. We find that the disk radius is constrained to the range 100 to 300 AU, depending on the steepness of the disk surface density distribution. The power law index of the dust opacity coefficient, β, is constrained to be 0.5 to 0.7. Since the models indicate that the disk is optically thin at millimeter wavelengths for radii greater than 8 AU, the contribution of an optically thick region to the emission is less than 10%. This implies that high optical depth or complex disk geometry cannot be the cause of the observed shallow millimeter spectral index. Instead, the new analysis supports the earlier suggestion that dust particles in the disk have grown to sizes as large as a few centimeters. The dust in the CQ Tauri system appears to be evolved much like that in the TW Hydra system, a well-studied pre-main-sequence star of similar age and lower mass. The survival of gas-rich disks with incomplete grain evolution at such old ages deserves further investigations.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/748c5e06d7bbba420f3a0e8234ce278300c2a471

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

CO emission from discs around isolated HAeBe and Vega-excess stars (2005, unknown): “An upper limit to the gaseous disc radius of 85 au was measured using interferometry (Mannings & Sargent, 2000), although Testi et al. (2003) resolved the dust continuum emission at 7mm, finding a radius of 100-200 au.”
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.”
Circumstellar Dust Disks in Taurus-Auriga: The Submillimeter Perspective (2005, background): “…observations of both young (e.g., Beckwith & Sargent 1991; Mannings 1994; Koerner, Chandler, & Sargent 1995) and old (e.g., Calvet et al. 2002; Hogerheijde et al. 2003) low mass disks, and particularly for those around the more massive Herbig Ae stars (Testi et al. 2001, 2003; Natta et al. 2004).”
High-Resolution Submillimeter Constraints on Circumstellar Disk Structure (2006, background): “Highresolution interferometric work has allowedmeasurements of , and therefore less ambiguous constraints on , adding further evidence for the presence of large grains in a variety of disks (e.g., Testi et al. 2001, 2003; Natta et al. 2004; Wilner et al. 2005; Rodmann et al. 2006).”
Dust grain growth in ρ-Ophiuchi protoplanetary disks (2010, background): “Wilner et al. (2000) and Testi et al. (2003) resolved the disks around TW Hya and CQ Tau PMS stars at 7 mm with the Very Large Array (VLA), confirming that the long-wave emission from these disks reveals the presence of cm-sized pebbles in the disk midplane.”
Forming Planetesimals in Solar and Extrasolar Nebulae (2009, background): “For a review of planetesimal formation that overlaps ours and covers some topics in greater detail, see the Les Houches lectures by Youdin (2008).”
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).”
Trapping dust particles in the outer regions of protoplanetary disks (2011, background): “…these questions is the observed grain growth to mm sized particles in the outer disk regions (Beckwith & Sargent (1991); Wilner et al. (2000, 2005); Testi et al. (2001, 2003); Andrews & Williams (2005); Rodmann et al. (2006); Natta et al. (2007); Isella et al. (2009); Lommen et al. (2009); Ricci…”
Dust Evolution and the Formation of Planetesimals (2016, background): “…the spectral indices of disks are usually much smaller than for ISM-like dust grains, indicating that dust grains in disk have grown to considerably larger sizes (Beckwith & Sargent 1991; Testi et al. 2003; Natta et al. 2004; Rodmann et al. 2006; Andrews & Williams 2007a; Ricci et al. 2010b,a).”
STRUCTURE AND EVOLUTION OF PRE-MAIN-SEQUENCE CIRCUMSTELLAR DISKS (2009, unknown): “…disks such as LkHα 330 (Brown et al. 2008), HD 163296 (Isella et al. 2007), AB Aur, MWC 480, DM Tau and LkCa 15 (Piétu et al. 2005, 2006, 2007), CQ Tau (Testi et al. 2003), DL Tau, UZ Tau, BP Tau and GM Aur (Simon et al. 2000), TW Hya (Wilner et al. 2000) and GG Tau (Guilloteau et al. 1999).”
The Disk Substructures at High Angular Resolution Project (DSHARP). V. Interpreting ALMA Maps of Protoplanetary Disks in Terms of a Dust Model (2018, unknown): “By inspecting the (sub-)millimeter spectral slope αmm we can learn something about the grain size distribution and the opacity law (e.g. Beckwith & Sargent 1991; Testi et al. 2003; 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.”
[O I] 6300 Å emission in Herbig Ae/Be systems: Signature of Keplerian rotation (2005, background): “For HAEBE stars of spectral type F, A and late-B, the evidence for a disk-like geometry of this circumstellar dust (e.g. Mannings & Sargent 1997; Testi et al. 2003; Piétu et al. 2003; Fuente et al. 2003; Natta et al. 2004) is generally accepted.”
A Submillimeter View of Circumstellar Dust Disks in ρ Ophiuchi (2007, background): “In those cases where the disk structure has been resolved and can be used to correct the colors ( ) for optically thick contamination, the typical opacity index is 1 (Testi et al. 2001, 2003; Rodmann et al. 2006; Lommen et al. 2007; Andrews & Williams 2007).”
A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, methodology): “Using this prescription, we collated L∗ estimates from the literature 7 (see Testi et al. 2003; Natta et al. 2004; Andrews et al. 2010, 2011, 2012, 2013; Cieza et al. 2012; Barenfeld et al. 2016; Cleeves et al. 2016) and computed posterior samples of 〈Td〉 for each posterior draw of brightness…”
Dust size distributions in coagulation/fragmentation equilibrium: numerical solutions and analytical fits (2010, background): “Indeed, the observational evidence suggests that growth up to cm-sizes is possible (e.g., Testi et al. 2003; Natta et al. 2004; Rodmann et al. 2006; Ricci et al. 2010).”
Dust properties of protoplanetary disks in the Taurus-Auriga star forming region from millimeter wavelengths (2009, methodology): “However, all available high angular resolution observations performed so far suggest that p ≤ 1.5 (e.g. Dutrey et al. 1996, Wilner et al. 2000, Kitamura et al. 2002, Testi et al. 2003, Andrews & Williams 2007, Isella et al. 2009, Andrews et al. 2009).”
Large dust particles in disks around T Tauri stars (2005, background): “Together with similar results for TW Hya, CQ Tau, and two Herbig Ae stars (HD 34282, HD 163296) (Calvet et al. 2002; Testi et al. 2003; Natta et al. 2004), a picture of grain growth to pebble-sized particles in disks around low- to intermediate-mass pre-main-sequence stars is emerging.”