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The formation of resonant pairs of planets in exoplanetary systems involvesplanetary migration in the protoplanetary disc. After a resonant capture, thesubsequent migration in this configuration leads to a large increase ofplanetary eccentricities if no damping mechanism is applied. This has led tothe conclusion that the migration of resonant planetary systems cannot occurover large radial distances and has to be terminated sufficiently rapidlythrough disc dissipation.  In this study, we investigate whether the presence of an inner disc mightsupply an eccentricity damping of the inner planet, and if this effect couldexplain the observed eccentricities in some systems. To investigate theinfluence of an inner disc, we first compute hydrodynamic simulations of giantplanets orbiting with a given eccentricity around an inner gas disc, andmeasure the effect of the latter on the planetary orbital parameters. We thenperform detailed long term calculations of the GJ 876 system. We also runN-body simulations with artificial forces on the planets mimicking the effectsof the inner and outer discs.  We find that the influence of the inner disc can not be neglected, and thatit might be responsible for the observed eccentricities. In particular, wereproduce quite well the orbital parameters of a few systems engaged in 2:1mean motion resonances: GJ 876, HD 73526, HD 82943 and HD 128311. Finally, wederive analytically the effect that the inner disc should have on the innerplanet to reach a specific orbital configuration with a given damping effect ofthe outer disc on the outer planet.

Influence of an inner disc on the orbital evolution of massive planets migrating in resonance