The time evolution of a system of two protoplanets
still embedded in a protoplanetary disk has been studied
viscous hydrodynamical simulations.
Resonant capture of the planets is seen, where
the order of the resonance depends on the initial spatial separation of the
planets, and the properties of the disk and the planets.
Resonant capture leads to a rise in the eccentricity and to an
alignment of the spatial orientation of orbits.
The numerical results are compared with the observed planetary
systems in mean motion resonance (GJ~876, HD~82943, and 55~Cnc).
We find that the forcing together of two planets by their parent disk
produces resonant configurations similar to those observed,
but that eccentricity damping greater than that obtained
in our hydrodynamic simulations is required to match the
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