  We study the effect of rotation during the collision between dust aggregates,
in order to address a mismatch between previous model calculations of Brownian
motion driven aggregation and experiments. We show that rotation during the
collision does influence the shape and internal structure of the aggregates
formed. The effect is limited in the ballistic regime when aggregates can be
considered to move on straight lines during a collision. However, if the
stopping length of an aggregate becomes smaller than its physical size,
extremely elongated aggregates can be produced. We show that this effect may
have played a role in the inner regions of the solar nebula where densities
were high.
