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In this paper we revise the model proposed by Rein et al. (2010) for theorigin of the HD45364 exoplanetary system, currently known to host two planetsclose to the 3/2 mean-motion commensurability (MMR). We show that, due to highsurface density of the protoplanetary disk needed for Type III migration, thismodel could only lead to planets in a quasi-resonant regime of motion, and thusnot consistent with the resonant configuration obtained by Correia et al.(2009). Although both resonant and quasi-resonant solutions are statisticallyindistinguishable with respect to radial velocity measurements, their distinctdynamical behaviour is intriguing. We use the semi-analytical model to confirmthe quantitative difference between two configurations. In order to form asystem evolving inside the 3/2 resonance, we develop a different model. Ourscenario includes an interaction between different (but slower) planetarymigration types, planet growth, and gap formation in the protoplanetary disk.The choice of the described evolutionary path was due to a detailed analysis ofthe structure of the phase space in the vicinity of the 3/2 MMR employingdynamical mapping techniques. The outcomes of our simulations are able toreproduce very closely the 3/2 resonant dynamics obtained from the best-fitpresented by Correia et al. (2009). In addition, varying the strength of theeccentricity damping, we can also simulate the quasi-resonant configurationsimilar to that in Rein et al. (2010). We furthermore show that our scenario isrobust with respect to the physical parameters involved in the resonancetrapping process. However, the confirmation of our scenario will be possibleonly with additional radial velocities measurements.

A new scenario for the origin of the 3/2 resonant system HD45364