The bulk composition of a planet can be roughly estimated using density measurements from observational data of radial velocity (planet mass) and planetary transits (planet radius Fulton & Petigura 2018 Zeng et al. The chemical composition of rocky planets is, among other factors such as the surface temperature or the presence of a magnetic field, an important parameter with respect to the habitability and the potential existence of extraterrestrial life. Subscribe to A&A to support open access publication. This article is published in open access under the Subscribe to Open model. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License ( ), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Their width can be adapted to reproduce gradual changes in planetary composition. Dynamic planetary accretion can be emulated well with any FZ model. Other element ratios are less influential. An increase in C/O from 0.1 to 0.7 results in a decrease of ∆ T c ≈ −100 K. The tested pressure range (10 −6 − 0.1 bar) corresponds to ∆ T c ≈ +350 K, and for −0.3 ≤ ≤ 0.4 we find ∆ T c ≈ +100 K. For most elements, it rises with p and metallicity. The T c is sensitive to variations in p and the abundance pattern. For common planet-building elements, we derive a T c that is within ±5 K of literature values, taking a wider spectrum of components into account. Our model reproduces the external results well in all tests. To derive the bulk compositions of planets, we explored three different planetary feeding-zone (FZ) models and compared their output to an external n-body simulation. To analyse the influence of the abundance pattern, key element ratios were varied, and the results were validated using solar neighbourhood stars. We assessed their change (∆ T c) as a result of p-variation between 10 −6 and 0.1 bar. We derived condensation temperatures for Solar System parameters with a simulation limited to the most common chemical species. Our T- p-dependent chemical equilibrium model is based on a Gibbs free energy minimisation. We also examined the bulk compositions of rocky planets around chemically diverse stars. For this purpose, we revisited condensation temperatures ( T c) as a means to study disk chemistry, and explored their sensitivity to variations in pressure ( p) and elemental abundance pattern. Our aim is to analyse how well a simplistic model can reproduce the main characteristics of rocky planet formation. We introduce ECCO PLANETS, an open-source Python code that simulates condensation in the protoplanetary disk. Equilibrium condensation simulations help us better understand the composition of the planets’ building blocks and their relation to the composition of their host star.Īims. ![]() The bulk composition of exoplanets cannot yet be directly observed. Institut für Astrophysik und Geophysik, Georg-August-Universität Göttingen,Į-mail: Zentrum Abteilung Geochemie und Isotopengeologie,Ĭentre for Earth Evolution and Dynamics, University of Oslo,Ĭontext. ![]() Astronomical objects: linking to databasesĪnina Timmermann 1, Yutong Shan 3, Ansgar Reiners 1 and Andreas Pack 2.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
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