arXiv 1107.20752011-07-11astro-ph.GA

星周盘中分子的化学历史

Chemical history of molecules in circumstellar disks

Ruud Visser, Ewine F. van Dishoeck, Steven D. Doty

备注：: 10 pages, 5 figures, to appear in the proceedings of IAU Symposium 280: "The Molecular Universe"
DOI：: 10.1017/S1743921311024938

摘要：

原行星盘的化学成分不仅取决于盘阶段的原位化学过程，还取决于气体和尘埃从出生包层吸积之前的历史。为了了解在行星形成时盘的化学成分，特别是在中平面，人们必须回到过去，追溯化学物质到坍缩形成盘和中心恒星的分子云。在这里，我们提出了一个新的天体化学模型，旨在做到这一点。该模型在两个维度上遵循核心坍缩和盘形成，这是对旧坍缩模型的关键升级。我们预测化学分层的磁盘由于不同的物理条件下遇到沿不同的流线。我们认为，盘包络吸积冲击不发挥显着的作用，在崩溃阶段结束时，在磁盘中的材料。最后，我们的模型表明，复杂的有机物种在20至40 K的温度下形成的颗粒表面上，而不是在气相中在T>100 K的热科里诺。

英文摘要：

The chemical composition of a protoplanetary disk is determined not only by in situ chemical processes during the disk phase, but also by the history of the gas and dust before it accreted from the natal envelope. In order to understand the disk's chemical composition at the time of planet formation, especially in the midplane, one has to go back in time and retrace the chemistry to the molecular cloud that collapsed to form the disk and the central star. Here we present a new astrochemical model that aims to do just that. The model follows the core collapse and disk formation in two dimensions, which turns out to be a critical upgrade over older collapse models. We predict chemical stratification in the disk due to different physical conditions encountered along different streamlines. We argue that the disk-envelope accretion shock does not play a significant role for the material in the disk at the end of the collapse phase. Finally, our model suggests that complex organic species are formed on the grain surfaces at temperatures of 20 to 40 K, rather than in the gas phase in the T>100 K hot corino.

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