C（n=2-10）、C（n =2-4）H和C3H2中性和阳离子物质的cosmic ray解离、光解离和解离重组的统计通用分支比
Statistical universal branching ratios for cosmic ray dissociation, photodissociation, and dissociative recombination of the C(n=2-10), C(n=2-4)H and C3H2 neutral and cationic species
摘要：
电子激发态分子的碎裂分支比对于气相星际化学的模拟是至关重要的。尽管在过去的二十年中已经进行了实验和理论上的努力，但仍然非常缺乏关于许多分子如Cn、CnH或C3 H2的这些量的详细信息。我们的目标是提供天体化学数据库与更现实的分支比的Cn（n=2至10），CnH（n=2至4），和C3 H2分子的电子激发的解离复合，光解，或宇宙射线过程中，没有详细的计算或测量存在于文献中。采用高速碰撞的逆运动学方法测量了电子激发态Cn（n=2 ~ 10）、CnH（n=2 ~ 4）和C3 H2分子的完整碎裂模式。解离的分支比由这些实验推导。全套的分支比被用作化学模型的新输入，并且在描述致密冷金牛座分子云-1和光子主导的马头区域的天体化学网络中观察到分支比修改效应。在这项工作中得到的分支比和其他类型的实验之间的比较显示出良好的一致性。它被解释为碎裂的统计行为的签名。我们得到的分支比导致C3产量的增加，以及更大的分散的子片段。在马头星云的光子主导区域模型中引入这些新值增加了C3和C3 H的丰度，但在视觉消光Av小于4时降低了较大Cn和碳氢化合物的丰度。
英文摘要：
Fragmentation branching ratios of electronically excited molecular species are of first importance for the modeling of gas phase interstellar chemistry. Despite experimental and theoretical efforts that have been done during the last two decades there is still a strong lack of detailed information on those quantities for many molecules such as Cn, CnH or C3H2. Our aim is to provide astrochemical databases with more realistic branching ratios for Cn (n=2 to 10), CnH (n=2 to 4), and C3H2 molecules that are electronically excited either by dissociative recombination, photodissociation, or cosmic ray processes, when no detailed calculations or measurements exist in literature. High velocity collision in an inverse kinematics scheme was used to measure the complete fragmentation pattern of electronically excited Cn (n=2 to 10), CnH (n=2 to 4), and C3H2 molecules. Branching ratios of dissociation where deduced from those experiments. The full set of branching ratios was used as a new input in chemical models and branching ratio modification effects observed in astrochemical networks that describe the dense cold Taurus Molecular Cloud-1 and the photon dominated Horse Head region. The comparison between the branching ratios obtained in this work and other types of experiments showed a good agreement. It was interpreted as the signature of a statistical behavior of the fragmentation. The branching ratios we obtained lead to an increase of the C3 production together with a larger dispersion of the daughter fragments. The introduction of these new values in the photon dominated region model of the Horse Head nebula increases the abundance of C3 and C3H, but reduces the abundances of the larger Cn and hydrocarbons at a visual extinction Av smaller than 4.
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