We computed the abundance of refractory elements in planetary bodies formed in stellar systems with solar chemical composition by combining models for chemical composition and planet formation. We also consider the formation of refractory organic compounds, which have been ignored in previous studies on this topic. We used the commercial software package HSC Chemistry in order to compute the condensation sequence and chemical composition of refractory minerals incorporated into planets. The problem of refractory organic material is approached with two distinct model calculations: the first considers that the fraction of atoms used in the formation of organic compounds is removed from the system (i.e. organic compounds are formed in the gas phase and are nonreactive); and the second assumes that organic compounds are formed by the reaction between different compounds that had previously condensed from the gas phase. Results show that refractory material represents more than 50 wt % of the mass of solids accreted by the simulated planets, with up to 30 wt % of the total mass composed of refractory organic compounds. Carbide and silicate abundances are consistent with C/O and Mg/Si elemental ratios of 0.5 and 1.02 for the Sun. Less than 1 wt % of carbides; pyroxene and olivine in similar quantities are formed. The model predicts planets that are similar in composition to those of the Solar system. It also shows that, starting from a common initial nebula composition, a wide variety of chemically different planets can form, which means that the differences in planetary compositions are due to differences in the planetary formation process. We show that a model in which refractory organic material is absent from the system is more compatible with observations. The use of a planet formation model is essential to form a wide diversity of planets in a consistent way.
The panchromatic JWST dayside spectrum of WASP-121 b reveals a refractory-rich formation
Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Heidelberg University（海德堡大学）；University College Cork（科克大学学院）；Aarhus University（奥胡斯大学）；University of Bristol（布里斯托大学）；University of Newcastle（纽卡斯尔大学）；Lund University（隆德大学）；Observatoire astronomique de l’Université de Genève（日内瓦大学天文台）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；Arizona State University（亚利桑那州立大学）；Espace pour la Vie（生命空间）；TU Graz（格拉茨工业大学）
The refractory fraction of phosphorus in planet-forming discs
Institute for Theoretical and Computation Physics, Graz University of Technology（格拉茨工业大学理论与计算物理研究所）；Tartu Observatory, University of Tartu（塔尔图大学塔尔图天文台）；Department of Physics and Astronomy, University College London（伦敦大学学院物理与天文学系）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）
Destruction of refractory carbon grains drives the final stage of proto-planetary disk chemistry
在这里，我们的目标是探索强C2 H线的起源，重新想象原行星盘的化学。有几个关键方面推动了我们的分析。首先，C2 H在年轻和年老的系统中都被检测到，暗示着一种长寿命的化学物质。第二，作为自由基，C2 H在不到1000年的时间内迅速被破坏。这两个陈述暗示了负责C2 H排放的化学必须主要在气相中并且必须处于平衡。结合新的和已发表的化学模型，我们发现，提高总挥发性（气体和冰）的C/O比是唯一的自然方式，以创造一个长寿命，高C2 H丰度。大部分\ce{C2H}存在于气体中，其Fuv/n-气体约为10^-7 G 0 cm ^3。为了提高挥发性C/O比，必须将额外的碳释放到气体中，以在贫氧条件下实现平衡化学。富碳颗粒的光烧蚀似乎是将C/O比提高到1.5以上的最直接方法，为长寿命的平衡循环提供动力。在Fuv/n-gas ~ 10^-7 G 0 cm ^3条件下，气体盘中存在高C/O比和高C2 H丰度的最佳条件区域正好位于卵石盘的外部，也可能位于盘隙中。因此，这个过程也可以解释在C2 H观测中看到的结构（暗示）。
Planets Around Solar Twins/Analogs (PASTA) I.: High precision stellar chemical abundance for 17 planet-hosting stars and the condensation temperature trend
