Size Dependence of the Bouncing Barrier in Protoplanetary Dust Growth

Abstract

Understanding the collisional behavior of dust aggregates is essential in the context of planet formation. It is known that low-velocity collisions of dust aggregates result in bouncing rather than sticking when the filling factor of colliding dust aggregates is higher than a threshold value. However, a large discrepancy between numerical and experimental results on the threshold filling factor was reported so far. In this study, we perform numerical simulations using soft-sphere discrete element methods and demonstrate that the sticking probability decreases with increasing aggregates radius. Our results suggest that the large discrepancy in the threshold filling factor may reflect the difference in the size of dust aggregates in earlier numerical simulations and laboratory experiments.

8 pages, 4 figures. Accepted for publication in ApJL

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Cited by in corpus (13)

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• The growth of super-large pre-planetary pebbles to an impact erosion limit
• Spatial distribution of crystalline silicates in protoplanetary disks: How to interpret mid-infrared observations
• Investigating the Bouncing Barrier with Collision Simulations of Compressed Dust Aggregates
• Clusters of tribocharged dust aggregates as pebbles in protoplanetary disks
• On the elastoplastic behavior in collisional compression of spherical dust aggregates
• Gas Phase Ions in Protoplanetary Disks from Collisions of Solids
• Exploring the conditions for forming planetesimals by the streaming instability and planetary systems by pebble accretion
• The Impact of Silicate Grain Coagulation on Millimeter Emission from Massive Protostellar Disks
• Oxygen Isotope Exchange Between Dust Aggregates and Ambient Nebular Gas
• Formation of Ryugu's parent planetesimal beyond the CO${}_2$ snow line from small pebbles: insights from thermal evolution modeling
• The Influence of the Fractal Dimension on Dust Evolution in Protoplanetary Disks
• Numerical Investigation on the Compressive Behavior of Hierarchical Granular Piles