  A major goal in the discovery and characterisation of exoplanets is to
identify terrestrial-type worlds that are similar to (or otherwise distinct
from) our Earth. Recent results have highlighted the importance of applying
devolatilisation -- i.e. depletion of volatiles -- to the chemical composition
of planet-hosting stars to constrain bulk composition and interiors of
terrestrial-type exoplanets. In this work, we apply such an approach to a
selected sample of 13 planet-hosting Sun-like stars, for which high-precision
photospheric abundances have been determined in the first paper of the series.
With the resultant devolatilised stellar composition (i.e. the model planetary
bulk composition) as well as other constraints including mass and radius, we
model the detailed mineralogy and interior structure of hypothetical,
habitable-zone terrestrial planets ("exo-Earths") around these stars. Model
output shows that most of these exo-Earths are expected to have broadly
Earth-like composition and interior structure, consistent with conclusions
derived independently from analysis of polluted white dwarfs. The exceptions
are the Kepler-10 and Kepler-37 exo-Earths, which we predict are strongly
oxidised and thus would develop metallic cores much smaller than Earth.
Investigating our devolatilisation model at its extremes as well as varying
planetary mass and radius (within the terrestrial regime) reveals potential
diversities in the interiors of terrestrial planets. By considering (i)
high-precision stellar abundances, (ii) devolatilisation, and (iii) planetary
mass and radius holistically, this work represents essential steps to explore
the detailed mineralogy and interior structure of terrestrial-type exoplanets,
which in turn are fundamental for our understanding of planetary dynamics and
long-term evolution.
