Streaming Instabilities in Protoplanetary Disks

By A. Youdin, J. Goodman. 2004

898 citations recorded by the source corpus.

Interpenetrating streams of solids and gas in a Keplerian disk produce a local, linear instability. The two components mutually interact via aerodynamic drag, which generates radial drift and triggers unstable modes. The secular instability does not require self-gravity, yet it generates growing particle-density perturbations that could seed planetesimal formation. Growth rates are slower than dynamical but faster than radial drift timescales. Growth rates, like streaming velocities, are maximized for marginal coupling (stopping times comparable to dynamical times). Fastest growth occurs when the solid-to-gas density ratio is order unity and feedback is strongest. Curiously, growth is strongly suppressed when the densities are too nearly equal. The relation between background drift and wave properties is explained by analogy with Howard's semicircle theorem. The three-dimensional, two-fluid equations describe a sixth-order (in the complex frequency) dispersion relation. A terminal velocity approximation allows simplification to an approximate cubic dispersion relation. To describe the simplest manifestation of this instability, we ignore complicating (but possibly relevant) factors such as vertical stratification, dispersion of particle sizes, turbulence, and self-gravity. We consider applications to planetesimal formation and compare our work to other studies of particle-gas dynamics.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/979d7b61c1763dc6ca78cd63e7f82aa1207babc8

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Citations in the corpus

The minimum-mass extrasolar nebula: in situ formation of close-in super-Earths (2012, background): “Recent work focuses on a combination of aerodynamic and gravitational instabilities to agglomerate particles (Youdin & Goodman 2005; Johansen et al. 2007; Bai & Stone 2010; and references therein) — or on pure gravitational instability of a vertically thin and dense dust layer (Lee et al. 2010a,b;…”
The Disk Substructures at High Angular Resolution Project (DSHARP). VI. Dust Trapping in Thin-ringed Protoplanetary Disks (2018, methodology): “Given that we do not compute the turbulent strength, but prescribe it, we should rely on the more fundamental volume density criterion of Youdin & Goodman (2005) to assess whether the dust in our model triggers the streaming instability or not.”
Dust Evolution and the Formation of Planetesimals (2016, background): “Smaller and larger particles require a higher mass-loading to trigger particle concentration (Youdin & Goodman 2005; Carrera et al. 2015).”
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).”
FORMATION OF KUIPER BELT BINARIES BY GRAVITATIONAL COLLAPSE (2010, background): “The streaming instability (Youdin & Goodman 2005) is a powerful concentration mechanism by which weak particle clumps perturb the gas flow in a way that increases their amplitude (Youdin & Johansen 2007, Johansen & Youdin 2007).”
RAPID COAGULATION OF POROUS DUST AGGREGATES OUTSIDE THE SNOW LINE: A PATHWAY TO SUCCESSFUL ICY PLANETESIMAL FORMATION (2012, background): “However, it is not obvious whether the clumps really experience the runaway collapse, since the growth timescal of theΩts ∼ 1 aggregates can be as short as one orbital period (see Section 5.1), which is comparable to the growth time of the streaming instability atΩts = 1 (Youdin & Goodman 2005).”
Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, background): “Since the back-reaction of dust on gas is strongest when dust-to-gas density ratio is of the order of unity (Youdin & Goodman 2005), a typical 20% accumulation of dust in the rings suggests that the creation of an individual ring in general may not be so relevant for the global disk dynamical…”
Multiple Disk Gaps and Rings Generated by a Single Super-Earth (2017, background): “Once dust is concentrated into rings, coagulation can be facilitated (e.g., Youdin & Shu 2002; Johansen et al. 2007; Pinilla et al. 2016), and instabilities such as the streaming instability (Youdin & Goodman 2005; Chiang & Youdin 2010) can be triggered.”
The nature of the TRAPPIST-1 exoplanets. (2018, background): “…et al. 2010; Birnstiel et al. 2012), 10-100 km-scale planetesimals form by a hydrodynamical instability (such as the streaming instability; (Youdin & Goodman 2005; Johansen et al. 2014)) in regions where the local solids-to-gas ratio is sufficiently high (Dra̧żkowska & Dullemond 2014;…”
DUST AND GAS IN THE DISK OF HL TAURI: SURFACE DENSITY, DUST SETTLING, AND DUST-TO-GAS RATIO (2015, background): “It has been suggested that, in this configuration, streaming instabilities will lead to very rapid clumping of dust particles (Youdin & Goodman 2005; Johansen & Youdin 2007), possibly providing a mechanism to grow boulders rapidly.”
Towards initial mass functions for asteroids and Kuiper Belt Objects (2010, background): “In the dense midplane layers of centimeter–meter size particles which can form in nonturbulent nebulae, the local gas is driven to near-Keplerian speeds and relative velocities between particles remain low enough for continued growth to planetesimal size to occur very rapidly, with or without the he”
Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations (2007, background): “These works find that streaming instabilities (Youdin and Goodman, 2005; Youdin and Johansen, 2007) lead to the clumping of particles, an effect our turbulent stirring models do not include.”
Ice Condensation as a Planet Formation Mechanism (2013, background): “The streaming instability causes particles to clump together due to the velocity difference between the particles and the gas in the disc, and planetesimals form through subsequent gravitational collapse (Youdin & Goodman, 2005; Johansen et al., 2007).”
Ring shaped dust accumulation in transition disks (2012, background): “When the dust-to-gas density ratio is close to unity, the feedback from the dust to the gas is non negligible and the growth timescales can be faster than the drift timescales (Youdin & Goodman 2005), potentially leading to planetesimal formation in the absence of self-gravity.”
Dynamics of pebbles in the vicinity of a growing planetary embryo: hydro-dynamical simulations (2012, methodology): “More specifically, this model builds on the recent planetesimal formation model (Youdin & Goodman 2005; Johansen et al. 2006, 2007, 2009) in which large planetesimals (with sizes from ∼100 up to ∼1000 km) form by the collapse of a self-gravitating clump of pebbles, concentrated to high densities by…”
Forming Planetesimals in Solar and Extrasolar Nebulae (2009, background): “20 SUMMARY AND OUTLOOK . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 21”