Dust growth in protoplanetary disks - a comprehensive experimental/theoretical approach

Abstract

More than a decade of dedicated experimental work on the collisional physics of protoplanetary dust has brought us to a point at which the growth of dust aggregates can - for the first time - be self-consistently and reliably modelled. In this article, the emergent collision model for protoplanetery dust aggregates (Güttler et al. 2010) as well as the numerical model for the evolution of dust aggregates in protoplanetary disks (Zsom et al. 2010) are reviewed. It turns out that, after a brief period of rapid collisional growth of fluffy dust aggregates to sizes of a few centimeters, the protoplanetary dust particles are subject to bouncing collisions, in which their porosity is considerably decreased. The model results also show that low-velocity fragmentation can reduce the final mass of the dust aggregates but that it does not trigger a new growth mode as discussed previously. According to the current stage of our model, the direct formation of kilometer-sized planetesimals by collisional sticking seems impossible so that collective effects, such as the streaming instability and the gravitational instability in dust-enhanced regions of the protoplanetary disk, are the best candidates for the processes leading to planetesimals.

to appear in Research in Astronomy and Astrophysics (RAA)

References in corpus (14)

• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? II. Introducing the bouncing barrier
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? I. Mapping the zoo of laboratory collision experiments
• Asteroids Were Born Big
• Closed-form expressions for particle relative velocities induced by turbulence
• Particle Clumping and Planetesimal Formation Depend Strongly on Metallicity
• Towards Initial Mass Functions for Asteroids and Kuiper Belt Objects
• High Velocity Dust Collisions: Forming Planetesimals in a Fragmentation Cascade with Final Accretion
• A representative particle approach to coagulation and fragmentation of dust aggregates and fluid droplets
• The Physics of Protoplanetesimal Dust Agglomerates. IV. Towards a Dynamical Collision Model
• New composite models of partially ionized protoplanetary disks
• The Physics of Protoplanetesimal Dust Agglomerates II. Low Velocity Collision Properties
• Collisions between equal sized ice grain agglomerates
• A coagulation-fragmentation model for the turbulent growth and destruction of preplanetesimals
• Numerical Simulations of Highly Porous Dust Aggregates in the Low-Velocity Collision Regime

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• The Formation and Dynamics of Super-Earth Planets
• Effects of photophoresis on the dust distribution in a 3D protoplanetary disc
• Inhibited Coagulation of Micron-size Dust Due to the Electrostatic Barrier
• Still water: dead zones and collimated ejecta from the impact of granular jets
• Carbon Depletion in the Early Solar System
• Toward a Population Synthesis of Disks and Planets I. Evolution of Dust with Entrainment in Winds and Radiation Pressure
• Rapid grain growth in post-AGB disc systems from far-infrared and sub-millimetre photometry
• Dissipation and adhesion hysteresis between (010) forsterite surfaces using molecular-dynamics simulation and the Jarzynski equality