  Most models of volatile delivery to accreting terrestrial planets assume that
the carriers for water are similar in water content to the carbonaceous
chondrites in our Solar System. Here we suggest that the water content of
primitive bodies in many planetary systems may actually be much higher, as
carbonaceous chondrites have lost some of their original water due to heating
from short-lived radioisotopes that drove parent body alteration. Using N-body
simulations, we explore how planetary accretion would be different if bodies
beyond the water line contained a water mass fraction consistent with chemical
equilibrium calculations, and more similar to comets, as opposed to the more
traditional water-depleted values. We apply this model to consider planet
formation around stars of different masses and identify trends in the
properties of Habitable Zone planets and planetary system architecture which
could be tested by ongoing exoplanet census data collection. Comparison of such
data with the model predicted trends will serve to evaluate how well the N-body
simulations and the initial conditions used in studies of planetary accretion
can be used to understand this stage of planet formation.
