With its large size, dense atmosphere, methane-based hydrological-like cycle, and diverse surface features, the Saturnian moon Titan is one of the most unique of the outer Solar System satellites. Study of the photochemically produced molecules in Titan’s atmosphere is critical in order to understand the mechanics of the atmosphere and, by extension, the interactions between atmosphere, surface, and subsurface water ocean. One example is propyne vapor, a photochemically produced species in Titan’s upper atmosphere expected to condense in Titan’s stratosphere at lower altitudes. Propyne may also be a trace species in Titan’s stratospheric co-condensed ice clouds detected by the Cassini Composite InfraRed Spectrometer. Bulk structural characterization of propyne ice is currently incomplete and is lacking in published laboratory Raman spectra and X-ray diffraction data. Here, we present a laboratory characterization of propyne ice, including the first published X-ray diffraction and Raman spectroscopy results for propyne ice.

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丙炔：在泰坦相关条件下测定物理性质和晶胞参数

土星卫星泰坦体积庞大，大气层稠密，具有类似甲烷的水文循环和多样的表面特征，是太阳系外最独特的卫星之一。研究土卫六大气中光化学产生的分子对于了解大气的力学以及进而了解大气、地表和地下水海洋之间的相互作用至关重要。一个例子是丙炔蒸气，这是土卫六高层大气中光化学产生的一种物质，预计会在土卫六较低海拔的平流层中凝结。丙炔也可能是卡西尼复合红外光谱仪检测到的土卫六平流层共凝结冰云中的痕量物质。丙炔冰的整体结构表征目前还不完整，并且缺乏已发表的实验室拉曼光谱和 X 射线衍射数据。在这里，我们介绍了丙炔冰的实验室表征，包括首次发表的丙炔冰的 X 射线衍射和拉曼光谱结果。