  The orbital parameters of the observed extrasolar planets differ strongly
from those of our own solar system. The differences include planets with high
masses, small semi-major axis and large eccentricities. We performed numerical
computations of embedded planets in disks and follow their mass growth and
orbital evolution over several thousand periods.
  We find that planets do migrate inwards on timescales of about $10^5$ years
on nearly circular orbits, during which they may grow up to about 5 Jupiter
masses. The interaction of the disk with several planets may halt the migration
process and lead to a system similar to the solar planetary system.
