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The statistical results of transiting planets show that there are two peaksaround 1.5 and 2.0 in the distribution of orbital period ratios. A large numberof planet pairs are found near the exact location of mean motion resonances(MMRs). In this work, we find out that the depletion and structures of gas diskplay crucial roles in driving planet pairs out of exact location of MMRs. Undersuch scenario, planet pairs are trapped into exact MMRs during orbitalmigration firstly and keep migrating in a same pace. The eccentricities can beexcited. Due to the existence of gas disk, eccentricities can be damped leadingto the change of orbital period. It will make planet pairs depart from theexact location of MMRs. With depletion timescales larger than 1 Myr, near MMRsconfigurations are formed easily. Planet pairs have higher possibilities toescape from MMRs with higher disk aspect ratio. Additionally, with weakercorotation torque, planet pairs can depart farther from exact location of MMRs.The final location of the innermost planets in systems are directly related tothe transition radius from optically thick region to inner optically thin disk.While the transition radius is smaller than 0.2 AU at the late stage of starevolution process, the innermost planets can reach around 10 days. Ourformation scenario is a possible mechanism to explain the formation of nearMMRs configuration with the innermost planet farther than 0.1 AU.

Departure from the Exact Location of Mean Motion Resonances Induced by the Gas Disk in the Systems Observed by Kepler