A Submillimeter View of Circumstellar Dust Disks in ρ Ophiuchi

By S. Andrews, Jonathan P. Williams. 2007

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We present new multiwavelength submillimeter continuum measurements of the circumstellar dust around 48 young stars in the ρ Ophiuchi dark clouds. Supplemented with previous 1.3 mm observations of an additional 99 objects from the literature, the statistical distributions of disk masses and submillimeter colors are calculated and compared to those in the Taurus-Auriga region. These basic submillimeter properties of young stellar objects in both environments are shown to be essentially identical. As with their Taurus counterparts, the ρ Oph circumstellar dust properties are shown to evolve along an empirical evolution sequence based on the infrared spectral energy distribution. The combined ρ Oph and Taurus Class II samples (173 sources) are used to set benchmark values for basic outer disk characteristics: Md ∼ 0.005 M☉, Md/M* ∼ 1% , and α ∼ 2 (where Fν ∝ να between 350 μm and 1.3 mm). The precision of these numbers is addressed in the context of substantial solid particle growth in the earliest stages of the planet formation process. There is some circumstantial evidence that disk masses inferred from submillimeter emission may be underestimated by up to an order of magnitude.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/d09980b300f7306cb2b3e222e53cf66bfe2f310b

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Citations in the corpus

Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 M☉ Main-Sequence Stars (2008, background): “…of dusty disks in the nearby Ophiuchus and Taurus-Auriga starforming regions indicate a 2Y3 ( 1) order of magnitude range in the masses (radii) of disks surrounding young stars with typical ages of 1Myr (e.g., Osterloh & Beckwith1995; Motte &André 2001; Andrews & Williams 2005, 2007a, 2007b).”
Protoplanetary Disks and Their Evolution (2011, methodology): “Further, the fraction of disks with at least a MMSN, 10MJup, within 60AU is similar, ∼ 11 − 13%, in Taurus, Ophiuchus, and Orion and, incidentally, comparable to the detection rate of Jupiter mass extrasolar planets (Mann & Williams 2009b).”
THE FORMATION MECHANISM OF GAS GIANTS ON WIDE ORBITS (2009, unknown): “The medium-mass nebulae hold 10% of the total system mass, consistent with disk masses derived from sub-mm observations (Andrews & Williams 2007).”
A simple model for the evolution of the dust population in protoplanetary disks (2012, background): “Also a constant dustto-gas ratio is usually assumed for deriving disk masses from dust continuum observations (e.g., Andrews & Williams 2005, 2007), which is one of the biggest sources of error in disk mass estimates.”
TIME EVOLUTION OF VISCOUS CIRCUMSTELLAR DISKS DUE TO PHOTOEVAPORATION BY FAR-ULTRAVIOLET, EXTREME-ULTRAVIOLET, AND X-RAY RADIATION FROM THE CENTRAL STAR (2009, methodology): “We as- sume that the initial disk mass (Mdisk) scales with the mass of the central star as indicated by observational studies (e.g., Andrews & Williams 2005, 2007) and specifically choose Mdisk(t = 0) = 0.1M∗.”
Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, background): “Especially grain growth could make this assumption partially invalid (e.g. Andrews & Williams 2007).”
On the theory of disc photoevaporation (2011, background): “Furthermore, given that the submillimetre observations show that most non-accreting stars (WTTs) are devoid of emission out to several hundreds of au (Duvert et al. 2000; Andrews & Williams 2005, 2007), the clearing must be correlated across all disc radii from 1 to 100 au.”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS. II. EXTENSION TO FAINTER SOURCES (2010, methodology): “Candidates were selected based on the single-dish photometry compiled by Andrews & Williams (2007b).”
RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, background): “Consider the millimeter-wave luminosities from disks in the nearby Tau and Oph associations (Andrews & Williams 2005b, 2007a; Cieza et al. 2010).”
THE BURST MODE OF ACCRETION AND DISK FRAGMENTATION IN THE EARLY EMBEDDED STAGES OF STAR FORMATION (2010, background): “…can explain observed T Tauri star mass accretion (Vorobyov & Basu 2007, 2008), but with late time disk masses that are about an order of magnitude greater than observational estimates (Vorobyov 2009a) which may really represent lower limits to the actual values (see e.g., Andrews & Williams 2007).”
EVOLUTIONARY SIGNATURES IN THE FORMATION OF LOW-MASS PROTOSTARS. II. TOWARD RECONCILING MODELS AND OBSERVATIONS (2005, background): “In a study of disks around Class II sources in Ophiuchus and Taurus, Andrews & Williams (2007) found a Md/M∗ distribution ranging from ∼ 10−3 − 0.2.”
The chemical history of molecules in circumstellar disks - I. Ices (2009, methodology): “The viscosity parameterα is kept constant at 10−2 (Dullemond et al. 2007; Andrews & Williams 2007b).”
Debris disks as signposts of terrestrial planet formation (2011, methodology): “…linear trend between the dust mass and the stellar mass such that the typical protoplanetary disk contains a few percent of the stellar mass (Andrews & Williams 2007a), which has important implications for the planet frequency as a function of stellar mass (Ida & Lin 2005; Raymond et al.…”
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, methodology): “…348 (Lee et al. 2011), and Upper Sco (Mathews et al. 2012) have systematically lower masses compared to Taurus (Andrews & Williams 2005) and Ophiuchus (Andrews & Williams 2007a), presumably due to evolutionary effects related to their environment, particle growth, and disk dispersal, respectively.”
A PARAMETRIC MODELING APPROACH TO MEASURING THE GAS MASSES OF CIRCUMSTELLAR DISKS (2013, background): “As an indication of the plausibility of the latter, we note that gas accretion rates integrated over protostellar ages are about an an order of magnitude higher than the disk masses derived from the dust continuum with a gas-todust ratio of 100 (Andrews & Williams 2007).”
PROSAC: a submillimeter array survey of low-mass protostars - II. The mass evolution of envelopes, disks, and stars from the class 0 through I stages (2009, methodology): “If compared at a common wavelength of 850µm, these three choices of parameters result in disk masses that agree within±15% from the middle value from Andrews & Williams (2007b). ring during the evolution of the young protostars could have an important effect on our derived disk masses and…”
Dust Evolution and the Formation of Planetesimals (2016, methodology): “A substantial improvement was provided by the Sub-millimeter Array (SMA) with high sensitivities and angular resolutions (Andrews & Williams 2007a,b; Andrews et al. 2010).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, methodology): “The SED used here was compiled from the optical survey by Wilking et al. (2005), the 2MASS database (Cutri et al. 2003), Spitzer photometry (Evans et al. 2003; Padgett et al. 2008), and integrated millimeter flux densities (350-1300 µm; Andrews & Williams 2007a,b).”
Dust grain growth in ρ-Ophiuchi protoplanetary disks (2010, methodology): “3.1, class II YSOs from the Andrews & Williams (2007a) catalogue.”