Numerical determination of the material properties of porous dust cakes

Abstract

The formation of planetesimals requires the growth of dust particles through collisions. Micron-sized particles must grow by many orders of magnitude in mass. In order to understand and model the processes during this growth, the mechanical properties, and the interaction cross sections of aggregates with surrounding gas must be well understood. Recent advances in experimental (laboratory) studies now provide the background for pushing numerical aggregate models onto a new level. We present the calibration of a previously tested model of aggregate dynamics. We use plastic deformation of surface asperities as the physical model to bring critical velocities for sticking into accordance with experimental results. The modified code is then used to compute compression strength and the velocity of sound in the aggregate at different densities. We compare these predictions with experimental results and conclude that the new code is capable of studying the properties of small aggregates.

arXiv commentAccepted for publication in A&A

References in corpus (13)

• Dust coagulation in protoplanetary disks: a rapid depletion of small grains
• Closed-form expressions for particle relative velocities induced by turbulence
• Formation of giant planets by fragmentation of protoplanetary disks
• The evolution of gravitationally unstable protoplanetary disks: fragmentation and possible giant planet formation
• Fragmentation of gravitationally unstable gaseous protoplanetary disks with radiative transfer
• The Thermal Regulation of Gravitational Instabilities in Protoplanetary Disks III. Simulations with Radiative Cooling and Realistic Opacities
• Dust sedimentation and self-sustained Kelvin-Helmholtz turbulence in protoplanetary disk mid-planes. I. Radially symmetric simulations
• The Internal Energy for Molecular Hydrogen in Gravitationally Unstable Protoplanetary Disks
• Testing Disk Instability Models for Giant Planet Formation
• Collisions between equal sized ice grain agglomerates
• Magnetic Aggregation I: Aggregation Dynamics and Numerical Modelling
• The influence of grain rotation on the structure of dust aggregates
• Shock propagation in a granular chain

Cited by in corpus (16)

• Dust coagulation and fragmentation in molecular clouds. I. How collisions between dust aggregates alter the dust size distribution
• Fluffy dust forms icy planetesimals by static compression
• The Physics of Protoplanetesimal Dust Agglomerates. III. Compaction in Multiple Collisions
• Cohesion of Amorphous Silica Spheres: Toward a Better Understanding of the Coagulation Growth of Silicate Dust Aggregates
• Erosion and the limits to planetesimal growth
• The Physics of Protoplanetesimal Dust Agglomerates. IV. Towards a Dynamical Collision Model
• Collisional evolution of dust aggregates. From compaction to catastrophic destruction
• Static compression of porous dust aggregates
• Erosion of dust aggregates
• Experiments on centimeter-sized dust aggregates and their implications for planetesimal formation
• Tensile Strength of Porous Dust Aggregates
• Compression Behaviour of Porous Dust Agglomerates
• Numerical Simulations of Highly Porous Dust Aggregates in the Low-Velocity Collision Regime
• Tensile & shear strength of porous dust agglomerates
• Formulating Compressive Strength of Dust Aggregates from Low to High Volume Filling Factors with Numerical Simulations
• The rotational disruption of porous dust aggregates from ab-initio kinematic calculations