论文标题
泰坦平流层的3.4μm吸收：乙烷，丙烷，丁烷和复杂的有机物的贡献
The 3.4 μm absorption of the Titan's stratosphere: contribution of ethane, propane, butane and complex hydrogenated organics
论文作者
论文摘要
卡西尼观察结果深入研究了由泰坦大气层所包含的复杂有机化学。其中，VIMS仪器在卡西尼（Cassini）的13年中执行的一系列太阳能掩体显示，以3.4 $ $ $ m的浓度为中心。泰坦大气中存在的几个分子在该波长区域中产生了光谱特征，但是它们的个人贡献很难解散。在这项工作中，我们使用辐射转移模型量化了各种分子物种对3.4 $ $ m频段的贡献。乙烷和丙烷是乐队的重要组成部分，但它们不足以完全适合形状，然后我们需要其他东西。多环芳烃（PAHS）和更复杂的多芳烃（如氢化的无定形碳（HAC））是最合理的候选者，因为它们富含C-H键。 PAHS签名已被检测到以上约900 km，并且被认为是气溶胶颗粒前体。各个光谱之间的高相似性阻碍了丰度的确定。
The complex organic chemistry harbored by the atmosphere of Titan has been investigated in depth by Cassini observations. Among them, a series of solar occultations performed by the VIMS instrument throughout the 13 years of Cassini revealed a strong absorption centered at 3.4 $μ$m. Several molecules present in Titan's atmosphere create spectral features in that wavelength region, but their individual contributions are difficult to disentangle. In this work, we quantify the contribution of the various molecular species to the 3.4 $μ$m band using a radiative transfer model. Ethane and propane are a significant component of the band but they are not enough to fit the shape perfectly, then we need something else. Polycyclic Aromatic Hydrocarbons (PAHs) and more complex polyaromatic hydrocarbons like Hydrogenated Amorphous Carbons (HACs) are the most plausible candidates because they are rich in C-H bonds. PAHs signature have already been detected above ~900 km, and they are recognized as aerosols particles precursors. High similarities between individual spectra impede abundances determinations.
