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Orbital mean motion resonances in planetary systems originate fromdissipative processes in disk-planet interactions that lead to orbitalmigration. In multi-planet systems that host giant planets, the perturbation ofthe protoplanetary disk strongly affects the migration of companion planets. Bystudying the well-characterized resonant planetary system around GJ 876 we aimto explore which effects shape disk-driven migration in such a multi-planetsystem to form resonant chains. We modelled the orbital migration of threeplanets embedded in a protoplanetary disk using two-dimensional locallyisothermal hydrodynamical simulations. We performed a parameter study byvarying the disk thickness, $\alpha$ viscosity, mass as well as the initialposition of the planets. Moreover, we have analysed and compared simulationswith various boundary conditions at the disk's inner rim. We find that due tothe high masses of the giant planets, substantial eccentricity can be excitedin the disk. This results in large variations of the torque acting on the outerlower-mass planet, which we attribute to a shift of Lindblad and corotationresonances due to disk eccentricity. Depending on disk parameters, themigration of the outer planet can be stopped in a non-resonant state. In othermodels, the outer planet is able to open a partial gap and to circularize thedisk again, later entering a 2:1 resonance with the most massive planet in thesystem to complete the observed Laplace resonance. Disk-mediated interactionsbetween planets due to spiral waves and excitation of disk eccentricity causedeviations from smooth inward migration of exterior lower mass planets.Self-consistent modelling of the disk-driven migration of multi-planet systemsis thus mandatory. Our results are compatible with a late migration of theoutermost planet into the resonant chain, when the giant planet pair already isin resonance.

Formation of a planetary Laplace resonance through migration in an eccentric disk - The case of GJ876