Simulating the 3.4-Micron Feature of Titan’s Haze

Bulletin of the Korean chemical society

Sang Joon Kim¹  C. Ennis¹  Y. S. Kim¹ 

关键词: Laboratory spectroscopy;    Infrared;    Astrochemistry;    Cosmic rays;    Solar system;   

DOI  :  

学科分类：化学（综合）

来源: Korean Chemical Society

【 摘 要 】

Four prominent features of Titan’s haze are found within the ‘3.4-μm’ absorption to be uniform with recent vertically resolved Cassini/VIMS spectra.1 These are absorptions at 2998 cm−1 (3.34 μm), 2968 cm−1 (3.37 μm), 2927 cm−1 (3.42 μm), and 2882 cm−1 (3.47 μm). A detailed fitting suggests that the 2998 cm−1 feature could originate from amorphous acetonitrile (CH3CN) carrying about 25% of integrated optical depth; the remaining features, which account for 75% of the integrated optical depth, could arise from a distinct triplet (C-H stretching) structure of radiolyzed hydrocarbons. An additional feature was possibly evidenced at altitudes higher than 300 km and attributable to ‘polymer-capped’ methane (CH4), significantly constraining the chemical composition of organic haze layers under Titan’s active radiation field.

【 授权许可】

Unknown