  Centimeter and meter sized solid particles in protoplanetary disks are
trapped within long lived high pressure regions, creating opportunities for
collapse into planetesimals and planetary embryos. We study the accumulations
in the stable Lagrangian points of a giant planet, as well as in the Rossby
vortices launched at the edges of the gap it carves. We employ the Pencil Code,
tracing the solids with a large number of interacting Lagrangian particles,
usually 100,000. For particles of 1 cm to 10 cm radii, gravitational collapse
occurs in the Lagrangian points in less than 200 orbits. For 5 cm particles, a
2 Earth mass planet is formed. For 10 cm, the final maximum collapsed mass is
around 3 Earth masses. The collapse of the 1 cm particles is indirect,
following the timescale of depletion of gas from the tadpole orbits. In the
edges of the gap vortices are excited, trapping preferentially particles of 30
cm radii. The rocky planet that is formed is as massive as 17 Earth masses,
constituting a Super-Earth. By using multiple particle species, we find that
gas drag modifies the streamlines in the tadpole region around the classical L4
and L5 points. As a result, particles of different radii have their stable
points shifted to different locations. Collapse therefore takes longer and
produces planets of lower mass. Three super-Earths are formed in the vortices,
the most massive having 4.4 Earth masses. We conclude that a Jupiter mass
planet can induce the formation of other planetary embryos in the outer edge of
its gas gap. Trojan Earth mass planets are readily formed, and although not
existing in the solar system, might be common in the exoplanetary zoo.
