Other
Scientific paper
Oct 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf..228w&link_type=abstract
EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.228
Other
Scientific paper
In order to understand the growth mechanisms of planetary bodies, one has to study collisions between small particles. Usually the relevant collision velocities depend on the particle size, smaller particles collide with smaller velocities than big ones. The initially (sub-) micrometer sized grains that are the building blocks of the bigger aggregates can be manipulated by gas jets that allow for a survey of a broad variety of velocities. Large aggregates collide with typical velocities of centimeters to meters per second or more, which can be achieved in the laboratory by using pendulums or monitoring two particles in free fall that have a relative velocity to each other. The growth of millimeter-sized dust aggregates is mainly determined by their behavior in collisions with velocities of a few millimeters per second. Due to gravity these velocities are nearly impossible to achieve in the laboratory. Therefore, we developed a microgravity setup that allows us to study collisions of about millimeter-sized particles at these low velocities. It is based on experiments by Heißelmann et al. (2010), who have conducted experiments where an ensemble of glass beads was injected into a flat chamber under microgravity conditions. Due to inelastic collisions among the glass beads the average velocity decreased over time (collisional cooling). As the coefficient of restitution, the ratio of the velocity of two colliding particles after and before a collision, is even lower for dust aggregates than for glass beads (Heißelmann et al., 2007), we expected this concept to work for dust as well.
Blum Jacques
Güttler Carsten
Weidling René
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