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We present an analytical and numerical study of the orbital migration andresonance capture of fictitious two-planet systems with masses in thesuper-Earth range undergoing Type-I migration. We find that, depending on theflare index and proximity to the central star, the average value of the periodratio, $P_2/P_1$, between both planets may show a significant deviation withrespect to the nominal value. For planets trapped in the 2:1 commensurability,offsets may reach values on the order of $0.1$ for orbital periods on the orderof $1$ day, while systems in the 3:2 mean-motion resonance (MMR) show muchsmaller offsets for all values of the semimajor axis. These properties are ingood agreement with the observed distribution of near-resonant exoplanets,independent of their detection method. We show that 2:1-resonant systems farfrom the star, such as HD82943 and HR8799, are characterized by very smallresonant offsets, while higher values are typical of systems discovered byKepler with orbital periods approximately a few days. Conversely, planetarysystems in the vicinity of the 3:2 MMR show little offset with no significantdependence on the orbital distance. In conclusion, our results indicate thatthe distribution of Kepler planetary systems around the 2:1 and 3:2 MMR areconsistent with resonant configurations obtained as a consequence of a smoothmigration in a laminar flared disk, and no external forces are required toinduce the observed offset or its dependence with the commensurability ororbital distance from the star.

Planetary migration and the origin of the 2:1 and 3:2 (near)-resonant population of close-in exoplanets