  Radial drift of solid particles in the protoplanetary disk is often invoked
as a threat to planet formation, as it removes solid material from the disk
before it can be assembled into planets. However, it may also concentrate
solids at particular locations in the disk, thus accelerating the coagulation
process. Planetesimals are thought to drift much faster in an eccentric disk,
due to their higher velocities with respect to the gas, but their drift rate
has only been calculated using approximate means. In this work, we show that in
some cases, previous estimates of the drift rate, based on a modification of
the results for an axisymmetric disk, are highly inaccurate. In particular, we
find that under some easily realized circumstances, planetesimals may drift
outwards, rather than inwards. This results in the existence of radii in the
disk that act as stable attractors of planetesimals. We show that this can lead
to a local enhancement of more than an order of magnitude in the surface
density of planetesimals, even when a wide dispersion of planetesimal size is
considered.
