Large dust particles in disks around T Tauri stars

By J. Rodmann, Th. Henning, C. Chandler, L. Mundy, D. Wilner. 2005

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We present 7-mm continuum observations of 14 low-mass pre-main-sequence stars in the Taurus-Auriga star-forming region obtained with the Very Large Array with ∼1.5 resolution and ∼0.3 mJy rms sensitivity. For 10 objects, the circumstellar emission has been spatially resolved. The large outer disk radii derived suggest that the emission at this wavelength is mostly optically thin. The millimetre spectral energy distributions are characterised by spectral indices α mm = 2.3 to 3.2. After accounting for contributions from free-free emission and corrections for optical depth, we determine dust opacity indices β in the range 0.5 to 1.6, which suggest that millimetre-sized dust aggregates are present in the circumstellar disks. Four of the sources with β > 1 may be consistent with submicron-sized dust as found in the interstellar medium. Our findings indicate that dust grain growth to millimetre-sized particles is completed within less than 1 Myr for the majority of circumstellar disks.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/278a0a6bfc0fddb9910b3806003d65b00869d99c

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Citations in the corpus

Multiwavelength analysis for interferometric (sub-)mm observations of protoplanetary disks - Radial constraints on the dust properties and the disk structure (2015, background): “…by emission from ionized gas, which is mostly relevant at longer wavelengths and is caused by thermal or nonthermal emission processes (e.g., free-free or gyro-synchrotron emission) from free electrons in the densest parts of a wind or the stellar corona (Rodmann et al. 2006; Ubach et al. 2012).”
Trapping dust particles in the outer regions of protoplanetary disks (2011, unknown): “…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 et al. (2010a, 2011); Guilloteau et al. (2011)) that…”
Protoplanetary Disks and Their Evolution (2011, background): “Surveys of Taurus disks have been carried out at 7mm by Rodmann et al. (2006) and at 3mm by Ricci et al. (2010b) who both find that the shallow SED slope generally extends to their observing wavelength and infer average opacity indices, 〈β〉 = 1, 0.6 respectively.”
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, unknown): “– 36 – 2005, 2007b; Rodmann et al. 2006; Cabrit et al. 2006; Bouy et al. 2008; Hughes et al. 2008, 2009; Schaefer et al. 2009; Isella et al. 2009, 2010, 2012; Hamidouche 2010; Öberg et al. 2010; Ricci et al. 2010, 2012, 2013; Andrews et al. 2011; Phan-Bao et al. 2011; Sandell et al. 2011; Cieza et…”
FIRST RESULTS FROM HIGH ANGULAR RESOLUTION ALMA OBSERVATIO NS TOWARD THE HL TAU REGION (2015, background): “At longer (cm) wavelengths, free-free emission from an outflow jet orthogonal to the disk plane contributes to the continuum (Wilner et al. 1996; Rodmann et al. 2006; Greaves et al. 2008; Carrasco-González et al. 2009).”
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).”
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.”
A dual-frequency sub-arcsecond study of proto-planetary disks at mm wavelengths: first evidence for radial variations of the dust properties (2011, methodology): “βm values have been reported for a number of sources in our sample by Rodmann et al. (2006) and Ricci et al. (2010).”
Rapid growth of gas-giant cores by pebble accretion (2012, background): “Dust continuum observations of young circumstellar discs around low-mass pre-main-sequence stars show growth of the dominant particle size to mm and cm sizes within less than 1 Myr (Testi et al. 2003; Wilner et al. 2005; Rodmann et al. 2006).”
STRUCTURE AND EVOLUTION OF PRE-MAIN-SEQUENCE CIRCUMSTELLAR DISKS (2009, background): “However, at the distance of the nearby star forming re- 1 gions (100-200 pc), the typical angular resolution of 1.5′′-3′′ (Rodmann et al. 2006; Andrews et al. 2007; Kitamura et al. 2002; Dutrey et al. 1996) could not constrain the detailed structure of disks, which typically have radii of only a…”
Cold Disks: Spitzer Spectroscopy of Disks around Young Stars with Large Gaps (2007, background): “There is general evidence for grain growth in disks from both mid-IR and millimeter data (Kessler-Silacci et al. 2006; Rodmann et al. 2006).”
Dust properties of protoplanetary disks in the Taurus-Auriga star forming region from millimeter wavelengths (2009, background): “…(9) Koerner et al. (1995); (10) Isella et al. (2009); (11) Kitamura et al. (2002); (12) Mundy et al. (1996); (13) Schaefer et al. (2009); (14) Ohashi et al. (1996); (15) Rodmann et al. (2006). of differences in the observations angular resolution, sensitivity, and methods for deriving the radius.”
A SPATIALLY RESOLVED INNER HOLE IN THE DISK AROUND GM AURIGAE (2009, background): “Grain growth is also somewhat inconsistent with the steep submillimeter slope observed by Rodmann et al. (2006) for the GM Aur system.”
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).”