Demographics of Planetesimals Formed by the Streaming Instability

Abstract

The streaming instability (SI) is a mechanism to aerodynamically concentrate solids in protoplanetary disks and facilitate the formation of planetesimals. Recent numerical modeling efforts have demonstrated the increasing complexity of the initial mass distribution of planetesimals. To better constrain this distribution, we conduct SI simulations including the self-gravity with hitherto the highest resolution. To subsequently identify all of the self-bound clumps, we develop a new clump-finding tool, PLanetesimal ANalyzer (\texttt{PLAN}). We then apply a maximum likelihood estimator to fit a suite of parameterized models with different levels of complexity to the simulated mass distribution. To determine which models are best-fitting and statistically robust, we apply three model selection criteria with different complexity penalties. We find that the initial mass distribution of clumps is not universal regarding both the functional forms and parameter values. Our model selection criteria prefer models different from those previously considered in the literature. Fits to multi-segment power law models break to a steeper distribution above masses close to 100 km collapsed planetesimals, similar to observed Kuiper Belt size distributions. We find evidence for a turnover in the low mass end of the planetesimal mass distribution in our high resolution run. Such a turnover is expected for gravitational collapse, but had not previously been reported.

accepted and published in ApJ (a typo in Table 6 (last column for VTPL) is fixed in this version (v4))

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Cited by in corpus (62)

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• The New Generation Planetary Population Synthesis (NGPPS). IV. Planetary systems around low-mass stars
• Thresholds for Particle Clumping by the Streaming Instability
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• Protoplanetary Disk Rings as Sites for Planetesimal Formation
• Streaming Instability in Turbulent Protoplanetary Disks
• Pebble-driven Planet Formation around Very Low-mass Stars and Brown Dwarfs
• How dust fragmentation may be beneficial to planetary growth by pebble accretion
• A Tale of Planet Formation: From Dust to Planets
• Turbulence Regulates the Rate of Planetesimal Formation via Gravitational Collapse
• Efficient planet formation by pebble accretion in ALMA rings
• Requirements for gravitational collapse in planetesimal formation --- the impact of scales set by Kelvin-Helmholtz and nonlinear streaming instability
• Rapid Formation of Massive Planetary Cores in a Pressure Bump
• How planets grow by pebble accretion II: Analytical calculations on the evolution of polluted envelopes
• Testing the Jeans, Toomre and Bonnor-Ebert concepts for planetesimal formation: 3D streaming instability simulations of diffusion regulated formation of planetesimals
• Streaming Instability with Multiple Dust Species: II. Turbulence and Dust-Gas Dynamics at Nonlinear Saturation
• Retrieving C and O Abundance of HR 8799 c by Combining High- and Low-Resolution Data
• Dust Settling and Clumping in MRI Turbulent Outer Protoplanetary Disks
• From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection
• Stratified and vertically-shearing streaming instabilities in protoplanetary disks
• System-level fractionation of carbon from disk and planetesimal processing
• An Analytical Theory for the Growth from Planetesimals to Planets by Polydisperse Pebble Accretion
• The hot main Kuiper belt size distribution from OSSOS
• Planetesimal Initial Mass Functions following Diffusion Regulated Gravitational Collapse
• From Dust to Planets I: Planetesimal and Embryo Formation
• How planets grow by pebble accretion IV: Envelope opacity trends from sedimenting dust and pebbles
• Reduced late bombardment on rocky exoplanets around M-dwarfs
• Dust growth, fragmentation and self-induced dust traps in PHANTOM
• Dust Settling Instability in Protoplanetary Discs
• Investigating Gravitational Collapse of a Pebble Cloud to form Transneptunian Binaries
• Direct Formation of Planetary Embryos in Self-Gravitating Disks
• Resilience of Planetesimal Formation in Weakly-Reinforced Pressure Bumps
• Constraints on planetesimal accretion inferred from particle-size distribution in CO chondrites
• Making the Solar System
• Streaming instabilities in accreting and magnetized laminar protoplanetary disks
• Prevalence of short-lived radioactive isotopes across exoplanetary systems inferred from polluted white dwarfs
• Dust Accumulation near the Magnetospheric Truncation of Protoplanetary Discs around T Tauri Stars
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• The detection of dust gap-ring structure in the outer region of the CR Cha protoplanetary disk
• Solving for the 2D Water Snowline with Hydrodynamic Simulations. Emergence of gas outflow, water cycle and temperature plateau
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• Planetesimal formation via the streaming instability with multiple grain sizes
• The cosmochemistry of planetary systems
• Shape models and spin states of Jupiter Trojans: Testing the streaming instability formation scenario
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• Superparticle Method for Simulating Collisions
• Erosion driven size-redistribution of protoplanetary disk solids and the onset of streaming Instability and Pebble Accretion
• Composition constraints of the TRAPPIST-1 planets from their formation
• Dust grain shattering in protoplanetary discs: collisional fragmentation or rotational disruption?
• On the Origin of the Pluto System
• The Limited Role of the Streaming Instability During Moon and Exomoon Formation
• Collisional heating of icy planetesimals. I. Catastrophic collisions
• Aeolian erosion in protoplanetary discs: How impactful it is on dust evolution?
• Planet Mass Function around M stars at 1-10 au: A Plethora of sub-Earth mass objects
• Evading the dust fragmentation barrier with the streaming instability in protoplanetary disks
• Dust Growth in ALMA Rings: II. Dusty Rossby Wave Instability
• The Luminosity Function of Ultra-Faint Trans-Neptunian Objects Detected by JWST
• Considering contact forces during the formation of planetesimals by gravitational collapse: mutual orbits, spin states, and shapes
• Magnitude of stable iron isotope fractionation limited by multiple stages of terrestrial core formation
• OSSOS finds an Exponential Cutoff in the Size Distribution of the Cold Classical Kuiper belt