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Context: In the early evolution of a planetary system, a pair of planets maybe captured in a mean motion resonance while still embedded in their nestingcircumstellar disk. Aims: The goal is to estimate the direction and amount ofshift in the semimajor axis of the resonance location due to the disk gravityas a function of the gas density and mass of the planets. The stability of theresonance lock when the disk dissipates is also tested. Methods: The orbitalevolution of a large number of systems is numerically integrated within athree-body problem in which the disk potential is computed as a series ofexpansion. This is a good approximation, at least over a limited amount oftime. Results: Two different resonances are studied: the 2:1 and the 3:2. Inboth cases the shift is inwards, even if by a different amount, when theplanets are massive and carve a gap in the disk. For super--Earths, the shiftis instead outwards. Different disk densities, Sigma, are considered and theresonance shift depends almost linearly on Sigma. The gas dissipation leads todestabilization of a significant number of resonant systems, in particular ifit is fast. Conclusions: The presence of a massive circumstellar disk maysignificantly affect the resonant behavior of a pair of planets by shifting theresonant location and by decreasing the size of the stability region. The diskdissipation may explain some systems found close to a resonance but not lockedin it.

Shifting of the resonance location for planets embedded in circumstellar disks