text: 440,152,1358763306895486985,1277975431723900936,Laura Rogers,"New co-authored paper on arXiv today! We find evidence that exoplanetary bodies have the same refractory composition as their host star <LINK> Some white dwarfs show evidence that they have accreted planetary material. Analysing their spectra reveals the bulk composition of the exoplanetary material that they have accreted. We analyse the abundances of a wide binary system consisting of a K-dwarf and a white dwarf which has accreted planetary material. As binary pairs are chemically homogeneous, the K-dwarf is used as a proxy for the progenitor composition of the white dwarf. The abundances of the K-dwarf and the planetary material polluting the atmosphere of the white dwarf are consistent with the hypothesis that exoplanetary bodies have the same refractory composition as their host stars. Check out the paper for more detail, discussions and caveats @MarcoMarco1822 Potentially! Although planet formation is very complicated. It may help to target certain stars when looking for potential exoplanets where life as we know it could exist! @MarcoMarco1822 We can use observations of polluted white dwarfs to infer if there was a core/mantle or even water sometimes, however, these planets have been destroyed so this makes it hard to find life there!",https://arxiv.org/abs/2102.02843,"Planets and stars ultimately form out of the collapse of the same cloud of gas. Whilst planets, and planetary bodies, readily loose volatiles, a common hypothesis is that they retain the same refractory composition as their host star. This is true within the Solar System. The refractory composition of chondritic meteorites, Earth and other rocky planetary bodies are consistent with solar, within the observational errors. This work aims to investigate whether this hypothesis holds for exoplanetary systems. If true, the internal structure of observed rocky exoplanets can be better constrained using their host star abundances. In this paper, we analyse the abundances of the K-dwarf, G200-40, and compare them to its polluted white dwarf companion, WD 1425+540. The white dwarf has accreted planetary material, most probably a Kuiper belt-like object, from an outer planetary system surviving the star's evolution to the white dwarf phase. Given that binary pairs are chemically homogeneous, we use the binary companion, G200-40, as a proxy for the composition of the progenitor to WD 1425+540. We show that the elemental abundances of the companion star and the planetary material accreted by WD 1425+540 are consistent with the hypothesis that planet and host-stars have the same true abundances, taking into account the observational errors. ","Host-star and exoplanet compositions: a pilot study usinga wide binary