Dust grain shattering in protoplanetary discs: collisional fragmentation or rotational disruption?

Abstract

In protoplanetary discs, the coagulation of dust grains into large aggregates still remains poorly understood. Grain porosity appears to be a promising solution to allow the grains to survive and form planetesimals. Furthermore, dust shattering has generally been considered to come only from collisional fragmentation; however, a new process was recently introduced, rotational disruption. We wrote a one-dimensional code that models the growth and porosity evolution of grains as they drift to study their final outcome when the two shattering processes are included. When simulating the evolution of grains in a disc model that reproduces observations, we find that rotational disruption is not negligible compared to the fragmentation and radial drift. Disruption becomes dominant when the turbulence parameter $α\lesssim 5\xtenpow{-4}$, if the radial drift is slow enough. We show that the importance of disruption in the growth history of grains strongly depends on their tensile strength.

arXiv commentPublished by MNRAS in Dec 2022, 14 pages, 14 figures

References in corpus (39)

• Streaming Instabilities in Protoplanetary Disks
• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Gas- and dust evolution in protoplanetary disks
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? I. Mapping the zoo of laboratory collision experiments
• Closed-form expressions for particle relative velocities induced by turbulence
• Radiative torques: Analytical Model and Basic Properties
• Rapid Coagulation of Porous Dust Aggregates Outside the Snow Line: A Pathway to Successful Icy Planetesimal Formation
• Protoplanetary Disk Turbulence Driven by the Streaming Instability: Linear Evolution and Numerical Methods
• Concentrating small particles in protoplanetary disks through the streaming instability
• A Parametric Modeling Approach to Measuring the Gas Masses of Circumstellar Disks
• Fluffy dust forms icy planetesimals by static compression
• Grain Retention and Formation of Planetesimals near the Snow Line in MRI-driven Turbulent Protoplanetary Disks
• Dust coagulation in protoplanetary disks: porosity matters
• Initial mass function of planetesimals formed by the streaming instability
• Numerical Modeling of the Coagulation and Porosity Evolution of Dust Aggregates
• Planetesimal formation around the snow line in MRI-driven turbulent protoplanetary disks
• Synthesis of the Morphological Description of Cometary Dust at Comet 67P
• Self-induced dust traps: overcoming planet formation barriers
• Cohesion of Amorphous Silica Spheres: Toward a Better Understanding of the Coagulation Growth of Silicate Dust Aggregates
• Rotational Disruption of Dust Grains by Radiative Torques in Strong Radiation Fields
• Formation and long-term evolution of 3D vortices in protoplanetary discs
• Demographics of Planetesimals Formed by the Streaming Instability
• An opening criterion for dust gaps in protoplanetary discs
• Revisiting the "radial-drift barrier" of planet formation and its relevance in observed protoplanetary discs
• The accumulation and trapping of grains at planet gaps: effects of grain growth and fragmentation
• Toroidal vortices and the conglomeration of dust into rings in protoplanetary discs
• Effect of dust radial drift on viscous evolution of gaseous disk
• Linear growth of streaming instability in pressure bumps
• Modeling dust growth in protoplanetary disks: The breakthrough case
• Tensile Strength of Porous Dust Aggregates
• How large are the monomers of dust aggregates in planet-forming disks?: Insights from quantitative optical and near-infrared polarimetry
• SPH simulations of grain growth in protoplanetary disks
• The tensile strength of dust aggregates consisting of small elastic grains: Constraints on the size of condensates in protoplanetary disks
• Evolution of porous dust grains in protoplanetary discs -- I. Growing grains
• Self-Induced Dust Traps Around Snow Lines in Protoplanetary Discs
• Dust growth, fragmentation and self-induced dust traps in PHANTOM
• Coagulation Instability in Protoplanetary Disks: A Novel Mechanism Connecting Collisional Growth and Hydrodynamical Clumping of Dust Particles
• Comparison of Viscosities from the Chapman-Enskog and Relaxation Time Methods
• Rotational Disruption of Porous Dust Aggregates due to Gas Flow in Protoplanetary Disks

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