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A major goal in the discovery and characterisation of exoplanets is toidentify terrestrial-type worlds that are similar to (or otherwise distinctfrom) our Earth. Recent results have highlighted the importance of applyingdevolatilisation -- i.e. depletion of volatiles -- to the chemical compositionof planet-hosting stars to constrain bulk composition and interiors ofterrestrial-type exoplanets. In this work, we apply such an approach to aselected sample of 13 planet-hosting Sun-like stars, for which high-precisionphotospheric abundances have been determined in the first paper of the series.With the resultant devolatilised stellar composition (i.e. the model planetarybulk composition) as well as other constraints including mass and radius, wemodel the detailed mineralogy and interior structure of hypothetical,habitable-zone terrestrial planets ("exo-Earths") around these stars. Modeloutput shows that most of these exo-Earths are expected to have broadlyEarth-like composition and interior structure, consistent with conclusionsderived independently from analysis of polluted white dwarfs. The exceptionsare the Kepler-10 and Kepler-37 exo-Earths, which we predict are stronglyoxidised and thus would develop metallic cores much smaller than Earth.Investigating our devolatilisation model at its extremes as well as varyingplanetary mass and radius (within the terrestrial regime) reveals potentialdiversities in the interiors of terrestrial planets. By considering (i)high-precision stellar abundances, (ii) devolatilisation, and (iii) planetarymass and radius holistically, this work represents essential steps to explorethe detailed mineralogy and interior structure of terrestrial-type exoplanets,which in turn are fundamental for our understanding of planetary dynamics andlong-term evolution.

Detailed chemical compositions of planet-hosting stars: II. Exploration of the interiors of terrestrial-type exoplanets