Ring shaped dust accumulation in transition disks

By P. Pinilla, M. Benisty, T. Birnstiel. 2012

300 citations recorded by the source corpus.

Context. Transition disks are believed to be the final stages of protoplanetary disks, during which a forming planetary system or photoevaporation processes open a gap in the inner disk, drastically changing the disk structure. From theoretical arguments it is expected that dust growth, fragmentation and radial drift are strongly influenced by gas disk structure, and pressure bumps in disks have been suggested as key features that may allow grains to converge and grow e ciently. Aims. We want to study how the presence of a large planet in a disk influences the growth and radial distribution of dust grains, and how observable properties are linked to the mass of the planet. Methods. We combine two-dimensional hydrodynamical disk simulations of disk-planet interactions with state-of-the-art coagulation/fragmentation models to simulate the evolution of dust in a disk which has a gap created by a massive planet. We compute images at di erent wavelengths and illustrate our results using the example of the transition disk LkCa15. Results. The gap opened by a planet and the long-range interaction between the planet and the outer disk create a single large pressure bump outside the planetary orbit. Millimeter-sized particles form and accumulate at the pressure maximum and naturally produce ring-shaped sub-millimeter emission that is long-lived because radial drift no longer depletes the large grain population of the disk. For large planet masses around 9 MJup, the pressure maximum and, therefore, the ring of millimeter particles is located at distances that can be more than twice the star-planet separation, creating a large spatial separation between the gas inner edge of the outer disk and the peak millimeter emission. Smaller grains do get closer to the gap and we predict how the surface brightness varies at di erent wavelengths.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c6b2bdcc3cca845a056a9cb265408f3bf400c2d1

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Citations in the corpus

Gas density drops inside dust cavities of transitional disks around young stars observed with ALMA (2015, background): “One important conclu- sion of Pinilla et al. (2012) is that the gas cavity radius (loca- tion of the planet) is expected to be up to a factor of 2 smaller than the dust cavity radius (location of the radial pressureb mp where the dust is trapped).”
Small vs. large dust grains in transitional disks: do different cavity sizes indicate a planet? - SAO 206462 (HD 135344B) in polarized light with VLT/NACO (2013, methodology): “Pinilla et al. (2012) have shown that the outer edge of the g seous halo carved out by a planet may not coincide with the location of the pressure bump generated by the same planet.”
Resolved gas cavities in transitional disks inferred from CO isotopologs with ALMA (2015, background): “…cavities are only an indirect consequence of planet clearing: a planet will lower the gas surface density along its orbit, creating a gas gap with a pressure bump at its outer edge where the millimeter-sized dust is trapped (e.g., Zhu et al. 2011; Dodson-Robinson & Salyk 2011; Pinilla et al. 2012).”
Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, background): “Pressure bumps could be created outside the orbit of a planet (e.g., Pinilla et al. 2012b) or the outer edge of a low-ionization region (the so-called dead zone; Flock et al. 2015).”
Pebble-isolation mass: Scaling law and implications for the formation of super-Earths and gas giants (2018, background): “The equilibrium between radial advection of dust particles and turbulent diffusion is achieved when (as also stated in Pinilla et al. 2012) vr,pρp − Dρg d dr = 0 , (17) where vr,p is the radial velocity of the pebbles, ρp the pebble density, ρg the gas density, D the diffusion coefficient…”
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.”
ALMA SURVEY OF LUPUS PROTOPLANETARY DISKS. I. DUST AND GAS MASSES (2016, background): “…of ongoing disk evolution, and their dust and gas distributions may be in some cases signposts of embedded planets clearing gaps in the disk (e.g., Pinilla et al. 2012; Pérez et al. 2014; van der Marel et al. 2015, 2016a; Canovas et al. 2015) Our ALMA continuum images show several Lupus disks…”
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).”
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).”
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). 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).”
Dust Evolution and the Formation of Planetesimals (2016, background): “Such vortices can trap dust particles (e.g., Barge & Sommeria 1995; Meheut et al. 2012; Lyra & Lin 2013; Raettig et al. 2015) in a similar way to pressure bumps (Paardekooper & Mellema 2004; Pinilla et al. 2012; Zhu et al. 2012; Birnstiel et al. 2013; Lyra & Lin 2013).”