Protoplanetary Disk Turbulence Driven by the Streaming Instability: Nonlinear Saturation and Particle Concentration

By Anders Johansen, A. Youdin. 2007

330 citations recorded by the source corpus.

We present simulations of the nonlinear evolution of streaming instabilities in protoplanetary disks. The two components of the disk, gas treated with grid hydrodynamics and solids treated as superparticles, are mutually coupled by drag forces. We find that the initially laminar equilibrium flow spontaneously develops into turbulence in our unstratified local model. Marginally coupled solids (that couple to the gas on a Keplerian timescale) trigger an upward cascade to large particle clumps with peak overdensities above 100. The clumps evolve dynamically by losing material downstream to the radial drift flow while receiving recycled material from upstream. Smaller, more tightly coupled solids produce weaker turbulence with more transient overdensities on smaller length scales. The net inward radial drift is decreased for marginally coupled particles, whereas the tightly coupled particles migrate faster in the saturated turbulent state. The turbulent diffusion of solid particles, measured by their random walk, depends strongly on their stopping time and on the solids-to-gas ratio of the background state, but diffusion is generally modest, particularly for tightly coupled solids. Angular momentum transport is too weak and of the wrong sign to influence stellar accretion. Self-gravity and collisions will be needed to determine the relevance of particle overdensities for planetesimal formation.

Subfields: Astronomy and Astrophysics, Fluid Flow and Transfer Processes

View Paper: https://www.semanticscholar.org/paper/2a0bac6c82ec7cdb8675264ba5196b90c26c93c0

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Citations in the corpus

Concentrating small particles in protoplanetary disks through the streaming instability (2016, background): “We note that Johansen & Youdin (2007) found that the morphological features of the streaming turbulence for tightly coupled particles in unstratified models are not axisymmetric, which can lead to stronger density fluctuations.”
Planetesimal formation near the snowline: in or out? (2017, background): “A promising mechanism to quickly form planetesimals directly from pebbles is streaming instability (Youdin & Goodman 2005; Johansen et al. 2007; Johansen & Youdin 2007).”
THE MASS AND SIZE DISTRIBUTION OF PLANETESIMALS FORMED BY THE STREAMING INSTABILITY. I. THE ROLE OF SELF-GRAVITY (2015, methodology): “The streaming instability has been studied analytically in the linear regime (Youdin & Goodman 2005; Youdin & Johansen 2007) and in the non-linear regime via numerical simulations (e.g., Johansen et al. 2007; Johansen & Youdin 2007; Bai & Stone 2010a).”
DUST AND GAS IN THE DISK OF HL TAURI: SURFACE DENSITY, DUST SETTLING, AND DUST-TO-GAS RATIO (2015, background): “ill prevent the dust grains from settling further. It has been suggested that in this conguration, streaming instabilities will lead to very rapid clumping of dust particles (Youdin and Goodman 2005; Johansen and Youdin 2007), possibly providing a mechanism to grow boulders rapidly. The increased ga”
Standing on the shoulders of giants : Trojan Earths and vortex trapping in low mass self-gravitating protoplanetary disks of gas and solids (2008, background): “…that when rocks and boulders migrate due to the drag force, they trigger a streaming instability that develops into a traffic jam in their migrating flow, with dramatic effects for the particle concentrations (Johansen et al. 2006b, Paardekooper 2006, Johansen & Youdin 2007, Balsara et al. 2008).”
Adding particle collisions to the formation of asteroids and Kuiper belt objects via streaming instabilities (2011, methodology): “We solve the standard shearing box equations for gas and particles (same as in Johansen & Youdin 2007, but with additional vertical gravity).”
Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks (2009, background): “1 (Youdin & Goodman 2005, Youdin & Johansen 2007, Johansen & Youdin 2007).”
Separating gas-giant and ice-giant planets by halting pebble accretion (2014, background): “Such concentrations can occur through the streaming instability, driven by the mutual drag between particles and gas (Youdin & Goodman 2005; Youdin & Johansen 2007; Johansen & Youdin 2007), or for example through the presence of vortices (Barge & Sommeria 1995) or pressure bumps (Whipple 1972).”
How to form planetesimals from mm-sized chondrules and chondrule aggregates (2015, background): “The streaming instability is another powerful mechanism for concentrating particles in localized dense clumps and preventing radial drift (Youdin & Goodman 2005; Johansen et al. 2007; Johansen & Youdin 2007; Bai & Stone 2010a).”
Forming Planetesimals in Solar and Extrasolar Nebulae (2009, background): “Johansen & Youdin (2007) perform nonlinear 3D simulations of the idealized SI using superparticles.”
Rapid growth of gas-giant cores by pebble accretion (2012, background): “In dead zones where the MRI does not operate, streaming instabilities can destabilize the relative motion between gas and particles (Youdin & Goodman 2005; Johansen & Youdin 2007; Bai & Stone 2010) and lead to the formation of dense filaments.”
RAPID COAGULATION OF POROUS DUST AGGREGATES OUTSIDE THE SNOW LINE: A PATHWAY TO SUCCESSFUL ICY PLANETESIMAL FORMATION (2012, background): “One important consequence of this instability is rapid clumping of marginally decoupled (Ωts ∼ 1) dust particles (e.g., Johansen & Youdin 2007; Johansen et al. 2007; Bai & Stone 2010a).”
Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations (2007, background): “Simulations have now begun to include the dynamical feedback of particles on gas dynamics (Johansen et al., 2006a; Johansen and Youdin, 2007).”
The Disk Substructures at High Angular Resolution Project (DSHARP). VI. Dust Trapping in Thin-ringed Protoplanetary Disks (2018, background): “Among the important aspects we have not treated in this paper are: the dust back-reaction onto the gas (e.g. Johansen & Youdin 2007; Gonzalez et al. 2017; Kanagawa et al. 2017b), the origin of the pressure bumps and/or gaps (e.g. Pinilla et al. 2012a; Béthune et al. 2016; Takahashi & Inutsuka 2016;…”
The structure of protoplanetary discs around evolving young stars (2014, background): “Several important growth and formation stages rely on detailed knowledge of the protoplanetary disc structure: – Growth of dust particles to pebble sized objects (Zsom et al. 2010; Birnstiel et al. 2012; Ros & Johansen 2013) Send offprint requests to: B. Bitsch, e-mail:bert@astro.lu.se – Movement of”