  We investigate the role of secular and mean motion resonances on the water
transport from a belt of icy asteroids onto planets or embryos orbiting inside
the circumprimary habitable zone (HZ) of a binary star system. In addition, the
host-star has an accompanying gas giant planet. For a comparison, we perform
two case studies where a secular resonance (SR) is located either inside the HZ
close to 1.0 au (causing eccentric motion of a planet or embryos therein) or in
the asteroid belt, beyond the snow line. In the latter case, a higher flux of
icy objects moving towards the HZ is expected. Collisions between asteroids and
objects in the HZ are treated analytically. Our purely dynamical study shows
that the SR in the HZ boosts the water transport; however, collisions can occur
at very high impact speeds. In this paper, we treat for the first time,
realistic collisions using a GPU 3D-SPH code to assess the water loss in the
projectile. Including the water loss into the dynamical results, we get more
realistic values for the water mass fraction of the asteroid during an impact.
We highlight that collisions occurring at high velocities greatly reduce the
water content of the projectile and thus the amount of water transported to
planets or embryos orbiting inside the HZ. Moreover, we discuss other effects
that could modify our results, namely the asteroid's surface rate recession due
to ice sublimation and the atmospheric drag contribution on the asteroids' mass
loss.
