热分子核中硫的旧汇：硫残留物的新研究
A new study of an old sink of sulfur in hot molecular cores: the sulfur residue
摘要：
在恒星形成区，硫的元素丰度似乎减少了一个数量级或更多。在过去的几年里，为了理解这种消耗背后的原因，已经进行了大量的观察和实验，但没有对高质量恒星形成核心的硫化学提供令人满意的解释。在这些区域中已经观察到几种含硫分子，但没有一种足够丰富以弥补气相缺陷。那么，这些隐藏的硫磺存在于何处呢？本文代表了一个进步，在我们的理解之间的相互作用的各种S-轴承物种。我们已经将最近的实验和理论数据纳入一个热分子核心的化学模型，以查看它们是否给出任何指示的身份硫汇在这些密集的区域。尽管我们的模型与许多含硫物质的固相和气相丰度都有合理的一致性，但我们发现，在最近的实验中检测到的硫残留物仅占我们模拟中可用硫的6%，而不是占硫预算的主导地位。
英文摘要：
Sulfur appears to be depleted by an order of magnitude or more from its elemental abundance in star-forming regions. In the last few years, numerous observations and experiments have been performed in order to to understand the reasons behind this depletion without providing a satisfactory explanation of the sulfur chemistry towards high-mass star-forming cores. Several sulfur-bearing molecules have been observed in these regions, and yet none are abundant enough to make up the gas-phase deficit. Where, then, does this hidden sulfur reside? This paper represents a step forward in our understanding of the interactions among the various S-bearing species. We have incorporated recent experimental and theoretical data into a chemical model of a hot molecular core in order to see whether they give any indication of the identity of the sulfur sink in these dense regions. Despite our model producing reasonable agreement with both solid-phase and gas-phase abundances of many sulfur-bearing species, we find that the sulfur residue detected in recent experiments takes up only ~6 per cent of the available sulfur in our simulations, rather than dominating the sulfur budget.
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