作者:Kanekazu Seki、Maoqi He、Renzhang Liu、Hideo Okabe
DOI:10.1021/jp952787z
日期:1996.1.1
the region from 190 to 255 nm with a resolution of 1 nm. The photochemistry of CA at 193.3 nm has been studied using a quadrupole mass spectrometer and a Fourier transform infrared spectrometer for product analysis. From the photolysis of HC3N−D2 and HC3N−CD4 mixtures and a plateau value of 0.3 for the quantum yield (QY) of DC3N (C3N + D2 → DC3N + D), it is concluded that the main dissociation process
氰基乙炔(CA)是泰坦大气中重要的次要成分,存在于星际介质中。已经在190nm至255nm的范围内以1nm的分辨率测量了CA的吸收截面。已经使用四极质谱仪和傅里叶变换红外光谱仪研究了193.3 nm处CA的光化学,用于产物分析。根据HC 3 N-D 2和HC 3 N-CD 4混合物的光解作用,DC 3 N(C 3 N + D 2 →DC 3 N + D)的量子产率(QY)的平稳值为0.3 ,结论是主要的离解过程是HC 3 N + hν→H + C ^ 3 0.30±0.05 QY和次要处理N是HC 3 N + ħ ν→c ^ 2 H带一个QY + CN等于或小于0.02。剩下的过程是形成亚稳态CA(三重态或卡宾)。CA的光解引起明显的压力降低和随之形成的薄雾。CA消失的QY为4.5±0.5,远高于联乙炔(QY = 2.0±0.5)和乙炔(QY = 2.3)。CA中快速形成的雾气可以解释在泰