CO2-ice Collisions: A New Experimental Approach

The coagulation of micrometer-sized particles marks the beginning of planet formation. For silicates a comprehensive picture already exists, which describes under which conditions growth can take place and which barriers must be overcome. With increasing distance to the central star volatiles freeze out and the collision dynamics is governed by the properties of the frozen volatiles. We present a novel experiment facility to analyze collisions of CO2 agglomerates consisting of micrometer-sized particles with agglomerate sizes up to 100 mu m. Experiments are conducted at temperatures around 100 K with collision velocities up to 3.4 m s(-1). Below impact velocities of around 0.1 m s(-1) sticking is observed and at collision velocities of 1 m s(-1) fragmentation also starts to occur. The experiments show that agglomerates of CO2 ice behave like silicate agglomerates with a comparable grain size distribution. Models developed to describe the collision dynamics of silicate dust can be applied to CO2 ice. This holds for the coefficient of restitution as well as for the threshold conditions for the transitions between sticking, bouncing, or fragmentation.

Automated summary

The coagulation of micrometer-sized particles marks the beginning of planet formation. Experimental results show that CO2 ice agglomerates behave similarly to silicate agglomerates, allowing for the application of collision dynamics models developed for silicate dust.