原太阳星云中作为难熔固体摇篮的岩石线
Rocklines as Cradles for Refractory Solids in the Protosolar Nebula
摘要：
在我们的太阳系中，类地行星和陨石物质呈现出各种各样的体成分。为了理解这种多样的组成，陨石的形成机制通常通过热力学方法来研究，忽略了整个原太阳星云的运输过程。在这里，我们调查所发挥的作用rocklines（冷凝/升华线的耐火材料）在最里面的区域的原太阳星云计算组成的粒子迁移到磁盘作为一个函数的时间。要做到这一点，我们利用一维吸积盘模型与处方的灰尘和蒸汽运输，升华和再冷凝的耐火材料（硅铁，顽火辉石，铁橄榄石，镁橄榄石，硫化铁，金属铁和镍）。我们发现，宇宙球粒，陨石球粒和陨石的大部分组成的多样性可以解释其形成接近岩石线，这表明固体物质集中在这些升华/冷凝前线附近。虽然我们的模型在很大程度上依赖于所考虑的物种数量和控制状态变化的热力学数据的可用性，但它表明岩石线在原太阳星云最内部区域的小型和大型天体的形成中发挥了重要作用。我们的模型提供了可能有助于水星大核心形成的机制的见解。
英文摘要：
In our solar system, terrestrial planets and meteoritical matter exhibit various bulk compositions. To understand this variety of compositions, formation mechanisms of meteorites are usually investigated via a thermodynamic approach that neglect the processes of transport throughout the protosolar nebula. Here, we investigate the role played by rocklines (condensation/sublimation lines of refractory materials) in the innermost regions of the protosolar nebula to compute the composition of particles migrating inward the disk as a function of time. To do so, we utilize a one-dimensional accretion disk model with a prescription for dust and vapor transport, sublimation and recondensation of refractory materials (ferrosilite, enstatite, fayalite, forsterite, iron sulfide, metal iron and nickel). We find that the diversity of the bulk composition of cosmic spherules, chondrules and chondrites can be explained by their formation close to rocklines, suggesting that solid matter is concentrated in the vicinity of these sublimation/condensation fronts. Although our model relies a lot on the number of considered species and the availability of thermodynamic data governing state changes, it suggests that rocklines played a major role in the formation of small and large bodies in the innermost regions of the protosolar nebula. Our model gives insights on the mechanisms that might have contributed to the formation of Mercury's large core.
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