| アブストラクト |
The physical processes driving the formation of planetesimals are still under debate. Current studies can explain the growth of dust particles to sizes of the order of millimeters. These are the typical sizes of chondrules of which we know that they were formed early in the solar system and that they were ubiquitous, accounting for up to 80% of the volume of chondrites. In CM2 chondrites all of these once molten particles as well as all other larger constituents are surrounded by dusty layers, whose origin as well as their influence on the collision behavior is not fully understood.
I will present our method to accrete dust onto chondrule analogs under different temperature conditions, referring to a freely floating chondrule in the early solar nebula. I will also report on a second experiment, in which we tested the influence of such dust rims on the collision behavior of chondrule analogs in free particle-particle collisions. |
