  Fine-grained rims (FGRs) are frequently found around chondrules in primitive
chondrites. The remarkable feature of FGRs is their submicron-sized and
non-porous nature. The typical thickness of FGRs around chondrules is 10--100
$\mu$m. Recently, a novel idea was proposed for the origin of FGRs: high-speed
collisions between chondrules and fine dust grains called the kinetic dust
aggregation process. Experimental studies revealed that (sub)micron-sized
ceramic particles can stick to a ceramic substrate in a vacuum when the impact
velocity is approximately in the range of 0.1--1 km/s. In this study, we
examine the possibility of FGR formation via kinetic dust aggregation in
chondrule-forming shock waves. When shock waves are created by undifferentiated
icy planetesimals, fine dust grains would be released from the planetary
surface due to evaporation of icy planetesimals. We consider the dynamics of
chondrules behind the shock front and calculate the growth of FGRs via kinetic
dust aggregation based on simple one-dimensional calculations. We found that
non-porous FGRs with the thickness of 10--100 $\mu$m would be formed in shock
waves around evaporating icy planetesimals.
