The influence of grain rotation on the structure of dust aggregates
arXiv:astro-ph/0601262 · doi:10.1016/j.icarus.2005.12.018
Abstract
We study the effect of rotation during the collision between dust aggregates, in order to address a mismatch between previous model calculations of Brownian motion driven aggregation and experiments. We show that rotation during the collision does influence the shape and internal structure of the aggregates formed. The effect is limited in the ballistic regime when aggregates can be considered to move on straight lines during a collision. However, if the stopping length of an aggregate becomes smaller than its physical size, extremely elongated aggregates can be produced. We show that this effect may have played a role in the inner regions of the solar nebula where densities were high.
15 pages, 6 figures, accepted for publication in Icarus, typos corrected
References in corpus (1)
Cited by in corpus (33)
- 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
- Dust coagulation in protoplanetary disks: porosity matters
- Three radial gaps in the disk of TW Hydrae imaged with SPHERE
- Free Collisions in a Microgravity Many-Particle Experiment. I. Dust Aggregate Sticking at Low Velocities
- Dust release and tensile strength of the non-volatile layer of cometary nuclei
- Numerical Modeling of the Coagulation and Porosity Evolution of Dust Aggregates
- Aggregate dust particles at comet 67P/Churyumov-Gerasimenko
- Dust evolution in protoplanetary discs and the formation of planetesimals. What have we learned from laboratory experiments?
- 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
- Collisional evolution of dust aggregates. From compaction to catastrophic destruction
- Static compression of porous dust aggregates
- Free Collisions in a Microgravity Many-Particle Experiment III: The Collision Behavior of sub-Millimeter-Sized Dust Aggregates
- Co-Accretion of Chondrules and Dust in the Solar Nebula
- The Physics of Protoplanetesimal Dust Agglomerates II. Low Velocity Collision Properties
- Dust growth in protoplanetary disks - a comprehensive experimental/theoretical approach
- Experimental Study on Bouncing Barriers in Protoplanetary Disks
- Clouds of Fluffy Aggregates: How They Form in Exoplanetary Atmospheres and Influence Transmission Spectra
- Understanding planet formation using microgravity experiments
- Fractal aggregates of sub-micron-sized grains in the young planet-forming disk around IM Lup
- Morphological effects on IR band profiles: Experimental spectroscopic analysis with application to observed spectra of oxygen-rich AGB stars
- Numerical Simulations of Highly Porous Dust Aggregates in the Low-Velocity Collision Regime
- Numerical determination of the material properties of porous dust cakes
- Super-Earths: A New Class of Planetary Bodies
- Analytic expressions for geometric cross-sections of fractal dust aggregates
- Millimeter Spectral Indices and Dust Trapping By Planets in Brown Dwarf Disks
- Formulating Compressive Strength of Dust Aggregates from Low to High Volume Filling Factors with Numerical Simulations
- Selective Aggregation Experiments on Planetesimal Formation and Mercury-Like Planets
- Clusters of tribocharged dust aggregates as pebbles in protoplanetary disks
- Models and Observational Predictions of Dust Traps in Protoplanetary Discs
- Interparticle normal force in highly porous granular matter during compression
- A Pathway for Collisional Planetesimal Growth in the Ice-Dominant Regions of Protoplanetary Disks