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tokens: simulations showed similar results. However, Chambers (2013) evidenced some differences related to the masses and the time-averaged eccentricities of the final planets. We believe that a more realistic treatment of the collisions should be included in future -body simulations. Such improvements will allow us to determine the orbital and physical properties of the planets formed in the simulations in greater detail. On the other hand, Marcus et al. (2010) presented results from smoothed particle hydrodynamics simulations of impacts between differentiated water(ice)-rock planets. From this, the authors analyzed the effects of late giant impacts on the final bulk abundance of water in super-Earths. Marcus et al. (2010) derived general laws, which should be incorporated into future -body calculations of planet formation to track the composition of growing planets in more detail. In the present work, we consider a snow line with a fixed position for each star. However, several works such as Ramirez Kaltenegger (2014) and Tian (2015) , calculated how the orbital distance of the HZ and the position of the snow line change throughout the pre-main-sequence (PMS) stage of the host star. In particular, for a 0.5 star, Ramirez Kaltenegger (2014) found that the snow line in the PMS moves inwards in the protoplanetary disk from 2 AU to 0.5 AU in a period of 200 Myr. Regardless of star type, all planets located at the inner edge of the main-sequence (MS) HZ receive stellar fluxes that exceed the runaway greenhouse threshold for at least part of the PMS stage, which results in the rapid evaporation of surface water. Triggering a runaway greenhouse does not ensure that a planet could not later become habitable because water could recondense afterwards. Planets orbiting at distances corresponding to the inner and outer MS HZ around a 0.5 star would lose up to 25 EOs and 0.5 EOs, respectively, and about 0.1 EOs are lost at the MS snow line. Assuming that a HZ and a snow line evolving in time may lead to changes in the final results obtained in the present work. Future works based on -body simulations should incorporate such effects to test the sensitivity of the results concerning the physical and dynamical properties of the HZ planets. It is also important to note that all our simulations were integrated for 150–200 Myr. Thus, the planetary systems obtained in the present work should be treated as systems of potential interest. It would be very interesting to analyze the long-period dynamical stability of the planets surviving in the HZ to clarify the distribution of these kind of exoplanets around low-mass stars. We believe that the results obtained in the present work lead to a better understanding about the planetary formation processes around M3- and M0-type stars in systems without gas giants. Future observational evidence will be necessary to test our theoretical models and to strengthen our knowledge about the population of terrestrial-like planets