Evidence of Fast Pebble Growth Near Condensation Fronts in the Hl Tau Protoplanetary Disk

Zhang, Ke; Blake, Geoffrey A.; Bergin, Edwin A.

doi:10.1088/2041-8205/806/1/l7

Cited by 398 publications

(416 citation statements)

References 41 publications

Supporting

Mentioning

402

Contrasting

Order By: Relevance

“…related to enhanced grain growth at snow lines of several dust spices (Zhang et al 2015), which should be consistent with the spherical grain size because the condensation growth leads grains to be larger spherical grains. On the other hand, if the submillimeter emission is coming from the fluffy aggregates, the Stokes number may be large enough to be decoupled from the gas.…”

Section: Stokes Numbersupporting

confidence: 55%

Grain Size Constraints on Hl Tau With Polarization Signature

Kataoka

Muto

Momose

et al. 2016

ApJ

119

147

View full text Add to dashboard Cite

The millimeter-wave polarization of the protoplanetary disk around HL Tau has been interpreted as the emission from elongated dust grains aligned with the magnetic field in the disk. However, the self-scattering of thermal dust emission may also explain the observed millimeter-wave polarization. In this paper, we report a modeling of the millimeter-wave polarization of the HL Tau disk with the self-polarization. Dust grains are assumed to be spherical and to have a power-law size distribution. We change the maximum grain size with a fixed dust composition in a fixed disk model to find the grain size to reproduce the observed signature. We find that the direction of the polarization vectors and the polarization degree can be explained with the self-scattering. Moreover, the polarization degree can be explained only if the maximum grain size is ∼150 μm. The obtained grain size from the polarization is different from that which has been previously expected from the spectral index of the dust opacity coefficient (a millimeter or larger) if the emission is optically thin. We discuss that porous dust aggregates may solve the inconsistency of the maximum grain size between the two constraints.

show abstract

Section: Stokes Numbersupporting

confidence: 55%

Grain Size Constraints on Hl Tau With Polarization Signature

Kataoka

Muto

Momose

et al. 2016

ApJ

119

147

View full text Add to dashboard Cite

show abstract

“…Table 1). The jump in the N 2 H + column density at the CO ice lines (at ≈15 and 80 au) is visible in both models but less pronounced in the Herbig Ae/Be disk The recent work of Zhang et al (2015) suggests that the locations of the dark rings visible in ALMA continuum observations of HL Tau (ALMA Partnership et al 2015) coincide with the expected ice line locations of several molecules. In particular, the locations of the H 2 O, NH 3 and CO ice lines agree well with the three most prominent dips in the radial surface brightness distribution.…”

Section: Ice Linesmentioning

confidence: 74%

The Gas Disk: Evolution and Chemistry

et al. 2016

View full text Add to dashboard Cite

Protoplanetary disks are the birthplaces of planetary systems. The evolution of the star-disk system and the disk chemical composition determines the initial conditions for planet formation. Therefore a comprehensive understanding of the main physical and chemical processes in disks is crucial for our understanding of planet formation. We give an overview of the early evolution of disks, discuss the importance of the stellar high-energy radiation for disk evolution and describe the general thermal and chemical structure of disks. Finally we provide an overview of observational tracers of the gas component and disk winds.

show abstract

“…At the typical densities of protoplanetary disks, water and CO condensate at temperatures between 130 and 150 K and 18 and 28 K, respectively [15,25]. At the temperatures of the HD 163296 disk (Fig.…”

Section: Prl 117 251101 (2016) P H Y S I C a L R E V I E W L E T T Ementioning

confidence: 98%

“…When this happens, the grain size shrinks affecting both its opacity and the gas drag. The combined result is an increase in the dust opacity right behind the frost line, which might result in the formation of bright emission rings in the microwave continuum emission [15,44].…”

Section: Prl 117 251101 (2016) P H Y S I C a L R E V I E W L E T T Ementioning

confidence: 99%

“…These include the aggregation of solids at the outer edge of disk regions characterized by low turbulence (e.g., [9][10][11][12][13][14]), variations in the dust opacity at the frost line of volatile elements [15,16], and gravitational perturbations caused by yet unseen giant planets [17]. In the first two cases, the observed structures might aid the formation of planetesimals by concentrating solid particles and preventing them from accreting onto the star [18,19].…”

mentioning

confidence: 99%

See 1 more Smart Citation

Searching for Baby Planets in a Star’s Dusty Rings

Williams

2016

Physics

View full text Add to dashboard Cite

We present Atacama Large Millimeter and Submillimeter Array observations of the protoplanetary disk around the Herbig Ae star HD 163296 that trace the spatial distribution of millimeter-sized particles and cold molecular gas on spatial scales as small as 25 astronomical units (A.U.). The image of the disk recorded in the 1.3 mm continuum emission reveals three dark concentric rings that indicate the presence of dust depleted gaps at about 60, 100, and 160 A.U. from the central star. The maps of the 12 CO, 13 CO, and C 18 O J ¼ 2 − 1 emission do not show such structures but reveal a change in the slope of the radial intensity profile across the positions of the dark rings in the continuum image. By comparing the observations with theoretical models for the disk emission, we find that the density of CO molecules is reduced inside the middle and outer dust gaps. However, in the inner ring there is no evidence of CO depletion. From the measurements of the dust and gas densities, we deduce that the gas-to-dust ratio varies across the disk and, in particular, it increases by at least a factor 5 within the inner dust gap compared to adjacent regions of the disk. The depletion of both dust and gas suggests that the middle and outer rings could be due to the gravitational torque exerted by two Saturn-mass planets orbiting at 100 and 160 A.U. from the star. On the other hand, the inner dust gap could result from dust accumulation at the edge of a magnetorotational instability dead zone, or from dust opacity variations at the edge of the CO frost line. Observations of the dust emission at higher angular resolution and of molecules that probe dense gas are required to establish more precisely the origins of the dark rings observed in the HD 163296 disk.

show abstract

Evidence of Fast Pebble Growth Near Condensation Fronts in the Hl Tau Protoplanetary Disk

Cited by 398 publications

References 41 publications

Grain Size Constraints on Hl Tau With Polarization Signature

Grain Size Constraints on Hl Tau With Polarization Signature

The Gas Disk: Evolution and Chemistry

Searching for Baby Planets in a Star’s Dusty Rings

Contact Info

Product

Resources

About