  In an attempt to select stars that can host planets with characteristics
similar to our own, we selected seven solar-type stars known to host planets in
the habitable zone and for which spectroscopic stellar parameters are
available. For these stars we estimated 'empirical' abundances of O, C, Mg and
Si, which in turn we used to derive the iron and water mass fraction of the
planet building blocks with the use of the model presented in Santos et al.
(2015). Our results show that if rocky planets orbit these stars they might
have significantly different compositions between themselves and different from
that of our Earth. However, for a meaningful comparison between the
compositional properties of exoplanets in the habitable zone and our own
planet, a far more sophisticated analysis (e.g. Dorn et al., 2017) of a large
number of systems with precise mass and radius of planets, and accurate
chemical abundances of the host stars. The work presented here is merely the
first humble step in this direction.
