How does the chemical composition of stars influence planet formation?

恒星的化学成分如何影响行星的形成?

基本信息

项目摘要

Protoplanetary discs, the birth places of planets, consist of mainly of gas and to a small fraction of dust. The dust grains can grow to pebbles (mm-cm in size) through coagulation and condensation of ices. These pebbles can then form planetesimals, which can then grow further by accreting other planetesimals or the small pebbles to form planetary embryos. Once the planetary embryos become big enough (several Earth masses), they can accrete a gaseous envelop to form eventually gas giants. During their growth, the planets migrate through the disc. This whole process is normally modeled in planet population synthesis simulations. However, several big questions remain.One of the big questions in planet formation is: where do the first planetesimals form? Recent simulations seem to indicate that the water ice line could be the prime location for this, also aided by condensation of water vapor, where usually a 50:50 ratio between water and rock is assumed in these simulations.In addition, planet formation depends strongly on the amount of dust available to grow to bigger objects. A higher dust-to-gas ratio or metallicity enhances growth and allows more efficient planetesimal and planet formation. The metallicity is determined through the host star abundance, mainly through the iron measurements, [Fe/H].In planet formation models in the past, a change of [Fe/H] implied an overall change of all elements in the same fashion. However, we know from galactic chemical tracing and evolution that different elements (e.g. C, O, Mg, Si, Fe) are enriched with different factors. As a consequence, different element ratios, e.g. Mg/Fe, Si/Fe, C/O have different slopes as function of [Fe/H].From chemical models it is clear that oxygen binds preferably with carbon compared to hydrogen. This implies that carbon binds large quantities of oxygen in CO and CO2, and only the remaining oxygen can form water. If the C/O ratio is large, it implies that less oxygen is available to form water. However, if less water is available, water condensation for grain growth and thus planetesimal formation might not work as efficiently. This proposal thus aims to answer the following questions by modeling the growth of planetesimals and subsequent planet formation including planetesimal and pebble accretion as well as planet migration in a single and N-body framework:1) How do the different volatile abundances (H2O, CO or CO2) influence the formation of pebbles and planetesimals?2) What influences do the overall abundances of elements have on the chemical composition of planets?3) Are the observable properties of formed planets different for host stars with different chemical composition?
原行星盘是行星的诞生地,主要由气体和一小部分尘埃组成。尘埃颗粒可以通过凝结和冰的凝结生长成鹅卵石(毫米-厘米大小)。这些卵石然后可以形成星子,然后通过吸积其他星子或小卵石形成行星胚胎来进一步生长。一旦行星胚胎变得足够大(几个地球质量),它们就可以吸积一个气体包层,最终形成气体巨星。在它们的生长过程中,行星会穿过圆盘迁移。整个过程通常在行星人口合成模拟中建模。然而,几个大问题仍然存在。行星形成中的一个大问题是:第一个星子是在哪里形成的?最近的模拟似乎表明,水冰线可能是最好的位置,也有助于水蒸气的冷凝,通常在这些模拟中假设水和岩石之间的比例为50:50。此外,行星的形成强烈依赖于可供成长为更大物体的尘埃量。更高的尘气比或金属丰度会促进生长,并允许更有效的微行星和行星形成。金属丰度是通过宿主星星的丰度来确定的,主要是通过铁的测量,[Fe/H]。在过去的行星形成模型中,[Fe/H]的变化意味着所有元素以相同的方式整体变化。然而,我们从银河系化学示踪和演化中知道,不同的元素(如C,O,Mg,Si,Fe)以不同的因子富集。因此,不同的元素比率,例如Mg/Fe、Si/Fe、C/O具有作为[Fe/H]的函数的不同斜率。从化学模型中可以清楚地看出,与氢相比,氧优选与碳结合。这意味着碳在CO和CO2中结合了大量的氧,只有剩余的氧可以形成水。如果C/O比大,则意味着可用于形成水的氧气较少。然而,如果可用的水较少,则用于晶粒生长的水冷凝以及由此的星子形成可能不会有效地工作。因此,该建议的目的是回答以下问题,通过模拟的星子的生长和随后的行星形成,包括星子和卵石吸积以及行星迁移在一个单一的和N体框架:1)如何不同的挥发性丰度(H2O,CO或CO2)影响卵石和星子的形成?2)元素的总体丰度对行星的化学成分有什么影响?3)对于具有不同化学成分的宿主恒星,形成的行星的可观测性质是否不同?

项目成果

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