Streaming Instability of Multiple Particle Species in Protoplanetary Disks

Abstract

The radial drift and diffusion of dust particles in protoplanetary disks affect both the opacity and temperature of such disks as well as the location and timing of planetesimal formation. In this paper, we present results of numerical simulations of particle-gas dynamics in protoplanetary disks that include dust grains with various size distributions. We consider three scenarios in terms of particle size ranges, one where the Stokes number ${\tau }_{\mathrm{s}}=10^{-1}-10^0$, one where ${\tau }_{\mathrm{s}}=10^{-4}-10^{-1}$ and finally one where ${\tau }_{\mathrm{s}}=10^{-3}-10^0$. Moreover, we consider both discrete and continuous distributions in particle size. In accordance with previous works we find in our multi-species simulations that different particle sizes interact via the gas and as a result their dynamics changes compared to the single-species case. The larger species trigger the streaming instability and create turbulence that drives the diffusion of the solid materials. We measure the radial equilibrium velocity of the system and find that the radial drift velocity of the large particles is reduced in the multi-species simulations and that the small particle species move on average outwards. We also vary the steepness of the size distribution, such that the exponent of the solid number density distribution, $\mathrm{d}N/\mathrm{d}a\propto a^{-q}$, is either $q=3$ or $q=4$. We measure the scale height of the particles and observe that small grains are stirred up well above the sedimented midplane layer where the large particles reside. Our measured diffusion and drift parameters can be used in coagulation models for planet formation as well as to understand relative mixing of the components of primitive meteorites (matrix, chondrules and CAIs) prior to inclusion in their parent bodies.

arXiv comment19 pages, 34 figures, 1 table, Accepted for publication in Astronomy & Astrophysics

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Cited by in corpus (29)

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• Including Dust Coagulation in Hydrodynamic Models of Protoplanetary Disks: Dust Evolution in the Vicinity of a Jupiter-mass Planet
• Demographics of Planetesimals Formed by the Streaming Instability
• Streaming Instability for Particle-Size Distributions
• Streaming Instability with Multiple Dust Species: I. Favourable Conditions for the Linear Growth
• Requirements for gravitational collapse in planetesimal formation --- the impact of scales set by Kelvin-Helmholtz and nonlinear streaming instability
• On the coexistence of the streaming instability and the vertical shear instability in protoplanetary disks
• Testing the Jeans, Toomre and Bonnor-Ebert concepts for planetesimal formation: 3D streaming instability simulations of diffusion regulated formation of planetesimals
• Polydisperse Streaming Instability I. Tightly coupled particles and the terminal velocity approximation
• Nucleation and growth of iron pebbles explains the formation of iron-rich planets akin to Mercury
• Rocklines as Cradles for Refractory Solids in the Protosolar Nebula
• Streaming Instability with Multiple Dust Species: II. Turbulence and Dust-Gas Dynamics at Nonlinear Saturation
• A $75\%$ Occurrence Rate of Debris Discs around F stars in the $\beta$ Pic Moving Group
• Hydrodynamical turbulence in eccentric circumbinary discs and its impact on the in situ formation of circumbinary planets
• Polydisperse Streaming Instability III. Dust evolution encourages fast instability
• Stratified and vertically-shearing streaming instabilities in protoplanetary disks
• Streaming instability of multiple particle species II -- Numerical convergence with increasing particle number
• An Analytical Theory for the Growth from Planetesimals to Planets by Polydisperse Pebble Accretion
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• A Smoking Gun for Planetesimal Formation: Charge Driven Growth into a New Size Range
• Morphological signatures induced by dust back reaction in discs with an embedded planet
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• Planetesimal formation via the streaming instability with multiple grain sizes
• Dust-gas dynamics driven by the streaming instability with various pressure gradients
• The effect of the streaming instability on protoplanetary disc emission at millimetre wavelengths
• Polydisperse Formation of Planetesimals: The dust size distribution in clumps
• Observation of aerodynamic instability in the flow of a particle stream in a dilute gas
• Erosion driven size-redistribution of protoplanetary disk solids and the onset of streaming Instability and Pebble Accretion