Streaming instability on different scales. I. Planetesimal mass distribution variability

Abstract

We present numerical simulations of dust clumping and planetesimal formation initiated by the streaming instability with self-gravity. We examine the variability in the planetesimal formation process by employing simulation domains with large radial and azimuthal extents and a novel approach of re-running otherwise identical simulations with different random initializations of the dust density field.We find that the planetesimal mass distribution and the total mass of dust that is converted to planetesimals can vary substantially between individual small simulations and within the domains of larger simulations. Our results show that the non-linear nature of the developed streaming instability introduces substantial variability in the planetesimal formation process that has not been previously considered and suggests larger scale dynamics may affect the process.

arXiv commentAccepted to MNRAS, 12 pages, 7 figures

References in corpus (41)

• SciPy 1.0--Fundamental Algorithms for Scientific Computing in Python
• Power-law distributions in empirical data
• Rapid planetesimal formation in turbulent circumstellar discs
• Streaming Instabilities in Protoplanetary Disks
• Nonlinear Outcome of Gravitational Instability in Cooling, Gaseous Disks
• Athena: A New Code for Astrophysical MHD
• A Major Asymmetric Dust Trap in a Transition Disk
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? II. Introducing the bouncing barrier
• FARGO: a fast eulerian transport algorithm for differentially rotating disks
• Asteroids Were Born Big
• Particle Clumping and Planetesimal Formation Depend Strongly on Metallicity
• The Disk Substructures at High Angular Resolution Project (DSHARP) VI: Dust trapping in thin-ringed protoplanetary disks
• Dynamics of Solids in the Midplane of Protoplanetary Disks: Implications for Planetesimal Formation
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. I. The Role of Self-Gravity
• Protoplanetary Disk Turbulence Driven by the Streaming Instability: Linear Evolution and Numerical Methods
• Dust Evolution and the Formation of Planetesimals
• Fluffy dust forms icy planetesimals by static compression
• Three-phase Interstellar medium in Galaxies Resolving Evolution with Star formation and Supernova feedback (TIGRESS): Algorithms, Fiducial model, and Convergence
• Planetesimal formation by sweep-up: How the bouncing barrier can be beneficial to growth
• Close-in planetesimal formation by pile-up of drifting pebbles
• Initial mass function of planetesimals formed by the streaming instability
• Adding particle collisions to the formation of asteroids and Kuiper belt objects via streaming instabilities
• Rubble Pile Asteroids
• The Effect of the Radial Pressure Gradient in Protoplanetary Disks on Planetesimal Formation
• Particle-Gas Dynamics with Athena: Method and Convergence
• Implementation of the Shearing Box Approximation in Athena
• Can dust coagulation trigger streaming instability?
• Resonant Drag Instabilities in protoplanetary disks: the streaming instability and new, faster-growing instabilities
• Evidence for universality in the initial planetesimal mass function
• The solar nebula origin of (486958) Arrokoth, a primordial contact binary in the Kuiper belt
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. II. The Effect of the Radial Gas Pressure Gradient
• Demographics of Planetesimals Formed by the Streaming Instability
• Impact splash chondrule formation during planetesimal recycling
• On the Feeding Zone of Planetesimal Formation by the Streaming Instability
• A concentration of centimeter-sized grains in the Oph IRS 48 dust trap
• Turbulence Regulates the Rate of Planetesimal Formation via Gravitational Collapse
• On the Numerical Robustness of the Streaming Instability: Particle Concentration and Gas Dynamics in Protoplanetary Disks
• Requirements for gravitational collapse in planetesimal formation --- the impact of scales set by Kelvin-Helmholtz and nonlinear streaming instability
• Gas Properties and Implications for Galactic Star Formation in Numerical Models of the Turbulent, Multiphase ISM
• Physical models of streaming instabilities in protoplanetary disks
• Origin of (2014) MU69-like Kuiper-belt contact binaries from wide binaries

Cited by in corpus (10)

• Bifurcation of planetary building blocks during Solar System formation
• Rapid Formation of Massive Planetary Cores in a Pressure Bump
• From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection
• Formation of Comets
• How planets grow by pebble accretion IV: Envelope opacity trends from sedimenting dust and pebbles
• Resilience of Planetesimal Formation in Weakly-Reinforced Pressure Bumps
• Are there any pristine comets? Constraints from pebble structure
• Planetesimal formation via the streaming instability with multiple grain sizes
• Takeout and Delivery: Erasing the Dusty Signature of Late-stage Terrestrial Planet Formation
• OSSOS finds an Exponential Cutoff in the Size Distribution of the Cold Classical Kuiper belt