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Exoplanet interior modelling usually makes the assumption that the elementalabundances of a planet are identical to those of its host star. Host stellarabundances are good proxies of planetary abundances, but only for refractoryelements. This is particularly true for terrestrial planets, as evidenced bythe relative differences in bulk chemical composition between the Sun and theEarth and other inner solar system bodies. The elemental abundances of a planethost star must therefore be devolatilised in order to correctly represent thebulk chemical composition of its terrestrial planets. Furthermore, nickel andlight elements make an important contribution alongside iron to the core ofterrestrial planets. We therefore adopt an extended chemical network of thecore, constrained by an Fe/Ni ratio of 18 $\pm$ 4 (by number). By applyingthese constraints to the Sun, our modelling reproduces the composition of themantle and core, as well as the core mass fraction of the Earth. We also applyour modelling to four exoplanet host stars with precisely measured elementalabundances: Kepler-10, Kepler-20, Kepler-21 and Kepler-100. If these starswould also host terrestrial planets in their habitable zone, we find that suchplanets orbiting Kepler-21 would be the most Earth-like, while those orbitingKepler-10 would be the least. To assess the similarity of a rocky exoplanet tothe Earth in terms of interior composition and structure, high-precision hoststellar abundances are critical. Our modelling implies that abundanceuncertainties should be better than $\sim$ 0.04 dex for such an assessment tobe made.

Enhanced constraints on the interior composition and structure of terrestrial exoplanets