Molecular Evolution in Interstellar Clouds. I : Ion Chemistry in Dense Clouds
Molecular Evolution in Interstellar Clouds. I : Ion Chemistry in Dense Clouds
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星际云中的分子演化。
DOI：
10.1143/ptp.62.936
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发表时间：
1979
影响因子：
--
通讯作者：
H. Suzuki
中科院分区：
文献类型：
--
作者：
H. Suzuki
分子丰度是使用化学方案随时间计算的，该化学方案旨在代表包含最多 2 个重原子（C、N、0、S 和 Si）的所有分子的演化特征，并由氢在颗粒上的表面重组和 234 种物质的 2884 气相反应组成。对于所采用的模型（nH=10'cm-•，T=30K，CH= w-" s1/H 原子），观测到的分子成功产生，并在 t= "-'2 X 1016s 时达到稳态丰度，这比稠密云的演化时间尺度更长。含碳分子（C-0 键中的碳除外）在 t= '""10 10 s 时具有峰值丰度，此时大多数 C 原子在形成 CO 分子时被消耗。 C/CO 比率是稠密云中分子演化的良好指标。
Molecular abundances are calculated time-dependently using a chemical scheme which is constructed to represent the evolutional feature of all molecules containing up to 2 heavy atoms (C, N, 0, S and Si) and consisted of the surface recombination of hydrogen on grains and2884gasphase reactions of 234 species. For the model adopted (nH=10'cm-•, T=30K, CH= w-" s1 per H atom), observed molecules are produced successfully and attain their steady-state abundances at t= "-'2 X 1016s, which is longer than the evolutional time scale of dense clouds. Molecules containing carbon (except carbon in C-0 bond) have peak abun dances at t= '""10 10 s, when most C atoms are consumed in forming CO molecules. The C/CO ratio is a good indicator of molecular evolution in dense clouds.