Trapping dust particles in the outer regions of protoplanetary disks

By P. Pinilla, T. Birnstiel, L. Ricci, C. Dullemond, A. Uribe, L. Testi, A. Natta. 2011

305 citations recorded by the source corpus.

In order to explain grain growth to mm sized particles and their retention in outer regions of protoplanetary disks, as it is observed at sub-mm and mm wavelengths, we investigate if strong inhomogeneities in the gas density profiles can slow down excessive radial drift and can help dust particles to grow. We use coagulation/fragmentation and disk-structure models, to simulate the evolution of dust in a bumpy surface density profile which we mimic with a sinusoidal disturbance. For different values of the amplitude and length scale of the bumps, we investigate the ability of this model to produce and retain large particles on million years time scales. In addition, we introduced a comparison between the pressure inhomogeneities considered in this work and the pressure profiles that come from magnetorotational instability. Using the Common Astronomy Software Applications ALMA simulator, we study if there are observational signatures of these pressure inhomogeneities that can be seen with ALMA. We present the favorable conditions to trap dust particles and the corresponding calculations predicting the spectral slope in the mm-wavelength range, to compare with current observations. Finally we present simulated images using different antenna configurations of ALMA at different frequencies, to show that the ring structures will be detectable at the distances of the Taurus Auriga or Ophiucus star forming regions.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/940db8094ac0bc755d0ba5f1574cd36560eb0ba0

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Citations in the corpus

On the diversity and statistical properties of protostellar discs (2018, background): “Tripathi et al. also point out that the scaling may be due to the migration and growth of solids in discs, and/or that it may be due to unresolved optically thick (dust) emission with filling factors of a few tens of percent (e.g. rings; Pinilla et al. 2012; Lorén-Aguilar & Bate 2015).”
Observational Signatures of Planets in Protoplanetary Disks I: Gaps Opened by Single and Multiple Young Planets in Disks (2014, methodology): “Our models provide a natural explanation to the recently discovered gap size dependence on wavelength, confirming previous results from literature (e.g. Pinilla et al. 2012).”
Ring shaped dust accumulation in transition disks (2012, background): “One possible solution to prevent the rapid inward drift and trap dust particles, is to consider pressure bumps (Klahr & Henning 1997; Fromang & Nelson 2005; Brauer et al. 2008; Johansen et al. 2009; Pinilla et al. 2012).”
SHADOWS CAST BY A WARP IN THE HD 142527 PROTOPLANETARY DISK (2014, methodology): “This parametric model also includes the effect of dust trapping, following the procedure described in Birnstiel et al. (2013) and Pinilla et al. (2012).”
Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud (2019, background): “Disk substructures may resolve this apparent contradiction, serving as the mechanism (e.g., dust traps, Pinilla et al. 2012; Dullemond et al. 2018) to hinder radial drift and preserve the disk materials in wide orbits.”
On planet formation in HL Tau (2015, background): “This begs the question of whether the gaps seen in HL Tau are genuine signatures of planet formation, or due to some oth r phenomena such as clumping (Lyra & Kuchner 2013), magnetic or Rossby-wave instabilities (Pinilla et al. 2012) or condensation fronts (Zhang et al. 2015).”
The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “Localized P modulations can slow or trap drifting solids (Whipple 1972; Pinilla et al. 2012a), perhaps concentrating them enough to trigger gravitational and/or streaming instabilities that rapidly convert pebbles to planetesimals (e.g., Youdin & Shu 2002; Youdin & Goodman 2005; Johansen et al.…”
The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation (2018, background): “…to studying observable disk features induced by planets (Wolf & D’Angelo 2005; Dodson-Robinson & Salyk 2011; Zhu et al. 2011; Gonzalez et al. 2012; Pinilla et al. 2012; Ataiee et al. 2013; Bae et al. 2016; Kanagawa et al. 2016; Rosotti et al. 2016; Isella & Turner 2018), including the…”
Multiwavelength analysis for interferometric (sub-)mm observations of protoplanetary disks - Radial constraints on the dust properties and the disk structure (2015, background): “…within 1 Myr (see also Laibe 2014) unless it is halted by the occurrence of dust traps (Whipple 1972; Weidenschilling 1977; Klahr & Henning 1997; Pinilla et al. 2012) or a different aerodynamic behavior when the grains are extremely fluffy aggregates (Okuzumi et al. 2012; Kataoka et al. 2013).”
RINGED SUBSTRUCTURE AND A GAP AT 1 au IN THE NEAREST PROTOPLANETARY DISK (2016, background): “The hypothesized solution to this conflict invokes substructure in the form of local gas pressure maxima, which slow or stop the migration of these particles and concentrate the solid densities to levels that might trigger efficient planetesimal growth (e.g., Whipple 1972; Pinilla et al. 2012).”
A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, background): “The remedy often proposed for this inconsistency is the presence of fine-scale, localized maxima in the radial pressure profile of the gas disk (e.g., Whipple 1972; Pinilla et al. 2012).”
Multiple Disk Gaps and Rings Generated by a Single Super-Earth (2017, background): “Although gas surface density contrasts generated by super-Earths may be modest, aerodynamic interactions between gas and dust can produce higher contrast features in dust (e.g., Rice et al. 2006; Pinilla et al. 2012b).”
The Disk Substructures at High Angular Resolution Project (DSHARP). VI. Dust Trapping in Thin-ringed Protoplanetary Disks (2018, background): “The dust trapping may explain their longevity, given the fact that dust grains tend to drift into the star on a short time scale in the absense of dust traps (Pinilla et al. 2012b).”
Direct mapping of the temperature and velocity gradients in discs Imaging the vertical CO snow line around IM Lupi (2017, background): “The radial concentration of dust grains depends strongly on the sub-Keplerian gas velocity, pressure gradients (e.g. Pinilla et al. 2012), and disc thermal structure (Laibe et al. 2012; Pinte & Laibe 2014).”
Survival of molecular gas in cavities of transition disks - I. CO (2013, methodology): “In an extension to this work, we plan to couple our model to the dust evolution models by Birnstiel et al. (2010, 2011, 2012b) and Pinilla et al. (2012b), in order to study the grain growth and planetary clearing scenario in more detail.”
The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures (2018, background): “A possible solution is that disk substructures impede radial drift, allowing large disk sizes to be maintained (e.g., Whipple 1972; Pinilla et al. 2012).”
Fluffy dust forms icy planetesimals by static compression (2013, background): “Several possibilities have been proposed to overcome these barriers (Johansen et al. 2007; Pinilla et al. 2012; Windmark et al. 2012; Lambrechts & Johansen 2012; Ros & Johansen 2013; Garaud et al. 2013).”
Global Simulations of the Inner Regions of Protoplanetary Disks with Comprehensive Disk Microphysics (2017, background): “In particular, dust grains always migrate toward higher pressure, leading to radial drift and particle trapping at pressure maxima; these theoretical predictions have found observational support (e.g., Pinilla et al. 2012; Birnstiel & Andrews 2014; Zhang et al. 2016).”