  We present a mechanism for chondrules to stick together by means of
compaction of a porous dust rim they sweep up as they move through the dusty
nebula gas. It is shown that dust aggregates formed out of micron-sized grains
stick to chondrules, forming a porous dust rim. When chondrules collide, this
dust can be compacted by means of rolling motions within the porous dust layer.
This mechanism dissipates the collisional energy, compacting the rim and
allowing chondrules to stick. The structure of the obtained chondrule-dust
agglomerates (referred to as compounds) then consists of three phases:
chondrules, porous dust, and dust that has been compacted by collisions.
Subsequently, these compounds accrete their own dust and collide with other
compounds. The evolution of the compound size distribution and the relative
importance of the phases is calculated by a Monte Carlo code. Growth ends, and
a simulation is terminated when all the dust in the compounds has been
compacted. Numerous runs are performed, reflecting the uncertainty in the
physical conditions at the chondrule formation time. It is found that compounds
can grow by 1-2 orders of magnitudes in radius, upto dm-sizes when turbulence
levels are low. However, relative velocities associated with radial drift form
a barrier for further growth. Earlier findings that the dust sweep-up by
chondrules is proportional to their sizes are confirmed. We contrast two
scenarios regarding how this dust evolved further towards the densely packed
rims seen in chondrites.
