Millimeter grains can form planetesimal-like clumps via the streaming instability in pressure bumps when the bump is only weakly reinforced, because particles then linger in the instability-favorable zone long enough for filaments to grow.
The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? I. Mapping the zoo of laboratory collision experiments
5 Pith papers cite this work. Polarity classification is still indexing.
5
Pith papers citing it
abstract
The growth processes from protoplanetary dust to planetesimals are not fully understood. Laboratory experiments and theoretical models have shown that collisions among the dust aggregates can lead to sticking, bouncing, and fragmentation. However, no systematic study on the collisional outcome of protoplanetary dust has been performed so far so that a physical model of the dust evolution in protoplanetary disks is still missing. We intend to map the parameter space for the collisional interaction of arbitrarily porous dust aggregates. This parameter space encompasses the dust-aggregate masses, their porosities and the collision velocity. With such a complete mapping of the collisional outcomes of protoplanetary dust aggregates, it will be possible to follow the collisional evolution of dust in a protoplanetary disk environment. We use literature data, perform own laboratory experiments, and apply simple physical models to get a complete picture of the collisional interaction of protoplanetary dust aggregates. In our study, we found four different types of sticking, two types of bouncing, and three types of fragmentation as possible outcomes in collisions among protoplanetary dust aggregates. We distinguish between eight combinations of porosity and mass ratio. For each of these cases, we present a complete collision model for dust-aggregate masses between 10^-12 and 10^2 g and collision velocities in the range 10^-4 to 10^4 cm/s for arbitrary porosities. This model comprises the collisional outcome, the mass(es) of the resulting aggregate(s) and their porosities. We present the first complete collision model for protoplanetary dust. This collision model can be used for the determination of the dust-growth rate in protoplanetary disks.
fields
astro-ph.EP 5years
2026 5representative citing papers
A semi-analytic model using elastoplastic contact mechanics and weakest-link fracture statistics reproduces the sticking-bouncing boundary from DEM simulations and places the bouncing barrier within ALMA-inferred size-velocity ranges for moderately porous aggregates.
Core accretion planet formation is theoretically feasible in high-mass post-AGB discs if local dust-to-gas ratios are enhanced and the streaming instability operates.
In gravitationally unstable discs, dust grains with Stokes numbers between about 0.1 and 1 are both most concentrated in spiral arms and least stirred up, making this the optimal window for direct dust collapse into planet cores.
Updated DALI models reproduce observed C2H2 fluxes with solar C/O and find the C2H2/H2O flux ratio sensitive to elemental abundances and small-grain abundance in planet-forming disk regions.
citing papers explorer
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Revisiting planetesimal formation from mm-sized grains in pressure bumps
Millimeter grains can form planetesimal-like clumps via the streaming instability in pressure bumps when the bump is only weakly reinforced, because particles then linger in the instability-favorable zone long enough for filaments to grow.
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A semi-analytic model of the bouncing barrier for protoplanetary dust aggregates
A semi-analytic model using elastoplastic contact mechanics and weakest-link fracture statistics reproduces the sticking-bouncing boundary from DEM simulations and places the bouncing barrier within ALMA-inferred size-velocity ranges for moderately porous aggregates.
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Second Generation Planet Formation in Post-AGB Discs - II: Dust Coagulation and Core Accretion
Core accretion planet formation is theoretically feasible in high-mass post-AGB discs if local dust-to-gas ratios are enhanced and the streaming instability operates.
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Dust trapping, collisional velocity and velocity dispersion in gravito-turbulent discs
In gravitationally unstable discs, dust grains with Stokes numbers between about 0.1 and 1 are both most concentrated in spiral arms and least stirred up, making this the optimal window for direct dust collapse into planet cores.
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Chemistry and IR emission of acetylene in planet-forming regions of T Tauri disks. Impact of elemental abundances and dust properties
Updated DALI models reproduce observed C2H2 fluxes with solar C/O and find the C2H2/H2O flux ratio sensitive to elemental abundances and small-grain abundance in planet-forming disk regions.