  We developed an experimental setup to test the hypothesis that accretionary
dust rims around chondrules formed in the solar nebula at elevated
temperatures. Our experimental method allows us to form dust rims around
chondrule-analogs while being levitated in an inert-gas flow. We used
micrometer-sized powdered San Carlos olivine to accrete individual dust
particles onto the chondrule-analog at a temperature of 1100{\deg}C. The
resulting dust-rims were analyzed by means of two different techniques: one
sample was investigated with non-destructive micro computer tomography, the
other with a scanning electron microscope. Both methods give very similar
results for the dust-rim structure and a mean dust-rim porosity of 60 percent,
demonstrating that both methods are equally well suited for sample analysis.
The chondrule-analog's bulk composition has no measurable effect on the
accretion efficiency of the dust. We measured the chemical composition of
chondrule-analog and dust-rim to check whether elemental exchange between the
tow components occurred. Such a reaction zone was not found, thus we can
experimentally confirm the sharp border between chondrules and dust-rims
described in the literature. The experimental dust-rim porosities and reported
porosities in carbonaceous and ordinary chondrites depend on the meteorite
type, indicating different degrees of compaction subsequent to parent
