A survey for circumstellar disks around young stellar objects

Beckwith, S.; Sargent, Anneila I.; Chini, R.; Guêsten, R.

doi:10.1086/115385

Cited by 1,468 publications

(1,632 citation statements)

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“…Over the past few decades, there have been numerous studies of nearby star-forming regions at millimeter wavelengths with the aim of measuring disk masses for large samples of disks, and this work has been accelerated in recent years by the power of ALMA to quickly survey large numbers of sources (e.g., Beckwith et al 1990;Osterloh & Beckwith 1995;Dutrey et al 1996;Andrews & Williams 2005, 2007Eisner et al 2008Eisner et al , 2016Mann & Williams 2010;Andrews et al 2013;Mann et al 2014;Ansdell et al 2016Ansdell et al , 2017Barenfeld et al 2016;Pascucci et al 2016). These surveys have tended to target the population of Class II protostar disks because they are no longer embedded in an envelope, and so estimates of their disk masses are more straightforward.…”

Section: Class I Versus Class Ii Disk Massesmentioning

confidence: 99%

“…1.3 mm cm 2 g −1 (e.g., Beckwith et al 1990) and T=20 K. We also assume a standard gas-to-dust ratio of 100.…”

Section: Class I Versus Class Ii Disk Massesmentioning

confidence: 99%

“…Disk masses are typically measured from their submillimeter flux, which, if tracing optically thin matter, is directly proportional to the amount of material present in the disk (e.g., Beckwith et al 1990). Class II disks are the easiest to study because, without a protostellar envelope, the entirety of the submillimeter flux can be attributed to disk emission.…”

Section: Introductionmentioning

confidence: 99%

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Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Sheehan

Eisner

2017

ApJ

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Class I protostars are thought to represent an early stage in the lifetime of protoplanetary disks, when they are still embedded in their natal envelope. Here we measure the disk masses of 10 Class I protostars in the Taurus Molecular Cloud to constrain the initial mass budget for forming planets in disks. We use radiative transfer modeling to produce synthetic protostar observations and fit the models to a multi-wavelength data set using a Markov Chain Monte Carlo fitting procedure. We fit these models simultaneously to our new Combined Array for Research in Millimeter-wave Astronomy 1.3 mm observations that are sensitive to the wide range of spatial scales that are expected from protostellar disks and envelopes so as to be able to distinguish each component, as well as broadband spectral energy distributions compiled from the literature. We find a median disk mass of  M 0.018 on average, more massive than the Taurus Class II disks, which have median disk mass of~ M 0.0025 . This decrease in disk mass can be explained if dust grains have grown by a factor of 75 in grain size, indicating that by the Class II stage, at a few Myr, a significant amount of dust grain processing has occurred. However, there is evidence that significant dust processing has occurred even during the Class I stage, so it is likely that the initial mass budget is higher than the value quoted here.

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Section: Class I Versus Class Ii Disk Massesmentioning

confidence: 99%

“…1.3 mm cm 2 g −1 (e.g., Beckwith et al 1990) and T=20 K. We also assume a standard gas-to-dust ratio of 100.…”

Section: Class I Versus Class Ii Disk Massesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Sheehan

Eisner

2017

ApJ

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“…We adopt the approach of Beckwith et al (1990) and assume a geometrically thin disk with power-law scalings with radius of the disk temperature and surface density, T(r) ϭ T 0 (r/r 0 ) Ϫq and ⌺(r) ϭ ⌺ 0 (r/r 0 ) Ϫp , where T 0 and ⌺ 0 are the dust temperature and mass surface density at the inner radius r 0 of the dust distribution. The optical depth is ϭ ⌺ / cos , where is the inclination of the disk axis to the line of sight and ϭ 0 ( / 0 ) ␤ is the specific dust opacity.…”

Section: Fitting Accretion Disk Modelsmentioning

confidence: 99%

“…There is now good evidence that a large fraction of young stellar objects have dense, dusty accretion disks (e.g., Beckwith et al 1990;Lada 1991). This is in accord with standard collapse models of star formation (e.g., Terebey, Shu, & Cassen 1984), which predict that systems older than 10 5 yr have centrifugally supported disks extending to 100 AU.…”

Section: Introductionmentioning

confidence: 99%

Accretion disks around class 0 protostars: The case of VLA 1623

Wilson¹,

Carlstrom²,

Lay³

et al. 1997

AIP Conference Proceedings

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Continuum emission at 220 and 355 GHz from the prototype class 0 source VLA 1623 has been detected using the James Clerk Maxwell Telescope-Caltech Submillimeter Observatory interferometer. Gaussian fits to the data place an upper limit of 70 AU on the half-width at half-maximum radius of the emission, which implies an upper limit of 1175 AU for the cutoff radius of the circumstellar disk in the system. In the context of existing collapse models, this disk could be magnetically supported on the largest scales and have an age of 16 ϫ 10 4 yr, consistent with previous suggestions that class 0 sources are quite young. The innermost region of the disk within 16 AU is likely to be in centrifugal support, which is likely large enough to provide a drive for the outflow according to current theoretical models. Alternatively, if 175 AU corresponds to the centrifugal radius of the disk, the age of the system is 12 ϫ 10 5 yr, closer to age estimates for class I sources.

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Planet–Planet Gravitational Scattering

Marzari

2010

Formation and Evolution of Exoplanets

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A survey for circumstellar disks around young stellar objects

Cited by 1,468 publications

References 0 publications

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Accretion disks around class 0 protostars: The case of VLA 1623

Planet–Planet Gravitational Scattering

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