  In this work is investigated the possibility of close-binary star systems
having Earth-size planets within their habitable zones. First, we selected all
known close-binary systems with confirmed planets (totaling 22 systems) to
calculate the boundaries of their respective habitable zones (HZ). However,
only eight systems had all the data necessary for the computation of the HZ.
Then, we numerically explored the stability within the habitable zones for each
one of the eight systems using test particles. From the results, we selected
five systems that have stable regions inside the habitable zones (HZ), namely
Kepler-34, 35, 38, 413 and 453. For these five cases of systems with stable
regions in the HZ, we perform a series of numerical simulations for planet
formation considering disks composed of planetary embryos and planetesimals,
with two distinct density profiles, in addition to the stars and host planets
of each system. We found that in the case of Kepler-34 and 453 systems no
Earth-size planet is formed within the habitable zones. Although planets with
Earth-like masses were formed in the Kepler-453, but they were outside the HZ.
In contrast, for Kepler-35 and 38 systems, the results showed that potentially
habitable planets are formed in all simulations. In the case of the Kepler-413
system, in just one simulation a terrestrial planet was formed within the
habitable zone.
