High Velocity Dust Collisions: Forming Planetesimals in a Fragmentation Cascade with Final Accretion

Abstract

In laboratory experiments we determine the mass gain and loss in central collisions between cm to dm-size SiO2 dust targets and sub-mm to cm-size SiO2 dust projectiles of varying mass, size, shape, and at different collision velocities up to ~56.5 m/s. Dust projectiles much larger than 1 mm lead to a small amount of erosion of the target but decimetre targets do not break up. Collisions produce ejecta which are smaller than the incoming projectile. Projectiles smaller than 1 mm are accreted by a target even at the highest collision velocities. This implies that net accretion of decimetre and larger bodies is possible. Independent of the original size of a projectile considered, after several collisions all fragments will be of sub-mm size which might then be (re)-accreted in the next collision with a larger body. The experimental data suggest that collisional growth through fragmentation and reaccretion is a viable mechanism to form planetesimals.

References in corpus (6)

• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Planetesimal Formation by Gravitational Instability
• Dust coagulation in protoplanetary disks: porosity matters
• The Physics of Protoplanetesimal Dust Agglomerates II. Low Velocity Collision Properties
• The influence of grain rotation on the structure of dust aggregates
• A coagulation-fragmentation model for the turbulent growth and destruction of preplanetesimals

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