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The Kepler mission has released ~4229 transiting planet candidates. There areapproximately 222 candidate systems with three planets. Among them, the periodratios of planet pairs near 1.5 and 2.0 reveal that two peaks exist for whichthe proportions of the candidate systems are ~7.0% and 18.0%, respectively. Inthis work, we study the formation of mean motion resonance (MMR) systems,particularly for the planetary configurations near 3:2 and 2:1 MMRs, and weconcentrate on the interplay between the resonant configuration and thecombination of stellar accretion rate, stellar magnetic field, speed ofmigration and additional planets. We perform more than 1000 runs by assuming asystem with a solar-like star and three surrounding planets. From thestatistical results, we find that under the formation scenario, the proportionsnear 1.5 and 2.0 can reach 14.5% and 26.0%, respectively. In addition, $\dotM=0.1\times 10^{-8} ~M_\odot ~{\rm yr^{-1}}$ is propitious toward the formationof 3:2 resonance, whereas $\dot M=2\times 10^{-8} ~M_\odot ~{\rm yr^{-1}}$contributes to the formation of 2:1 resonance. The speed-reduction factor oftype I migration $f_1\geq 0.3$ facilitates 3:2 MMRs, whereas $f_1\geq 0.1$facilitates 2:1 MMRs. If additional planets are present in orbits within theinnermost or beyond the outermost planet in a three-planet system, 3:2:1 MMRscan be formed, but the original systems trapped in 4:2:1 MMRs are not affectedby the supposed planets. In summary, we conclude that this formation scenariowill provide a likely explanation for Kepler candidates involved in 2:1 and 3:2MMRs.

Near 3:2 and 2:1 mean motion resonances formation in the systems observed by Kepler