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Aims. We study the formation and water delivery of planets in the habitablezone (HZ) around solar-type stars. In particular, we study different dynamicalenvironments that are defined by the most massive body in the system. Methods.First of all, a semi-analytical model was used to define the mass of theprotoplanetary disks that produce each of the five dynamical scenarios of ourresearch. Then, we made use of the same semi-analytical model to describe theevolution of embryos and planetesimals during the gaseous phase. Finally, wecarried out N-body simulations of planetary accretion in order to analyze theformation and water delivery of planets in the HZ in the different dynamicalenvironments. Results. Water worlds are efficiently formed in the HZ indifferent dynamical scenarios. In systems with a giant planet analog to Jupiteror Saturn around the snow line, super-Earths tend to migrate into the HZ fromoutside the snow line as a result of interactions with other embryos andaccrete water only during the gaseous phase. In systems without giant planets,Earths and super-Earths with high water by mass contents can either be formedin situ in the HZ or migrate into it from outer regions, and water can beaccreted during the gaseous phase and in collisions with water-rich embryos andplanetesimals. Conclusions. The formation of planets in the HZ with very highwater by mass contents seems to be a common process around Sun- like stars. Ourresearch suggests that such planets are still very efficiently produced indifferent dynamical environments. Moreover, our study indicates that theformation of planets in the HZ with masses and water contents similar to thoseof Earth seems to be a rare process around solar-type stars in the systemsunder consideration.

Planetary formation and water delivery in the habitable zone around solar-type stars in different dynamical environments