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Scattering And Absorption of Light in Planetary Regoliths
Published on: July 1, 2019
卡西尼UVIS恒星探测器探测了泰坦的大气层
Donald E Shemansky1, A Ian F Stewart, Robert A West
1Department of Aerospace Engineering, University of Southern California, University Park, Los Angeles, CA 90089, USA. dons@hippolyta.usc.edu
概括
卡西尼UVIS对泰坦进行了测量.
科学领域:
- 行星科学 行星科学
- 大气科学 大气科学
- 天体生物学 天体生物学
背景情况:
- 泰坦的大气组成和结构是理解其演变的关键.
- 之前的研究对上层大气层的化学成分提供了有限的数据.
研究的目的:
- 利用恒星隐蔽数据分析泰坦上层大气层的组成和温度结构.
- 识别和量化在不同高度存在的特定碳化合物和酸物种.
主要方法:
- 在泰坦飞越期间使用了卡西尼紫外线成像光谱仪 (UVIS).
- 从两颗背景恒星穿过泰坦大气层观察到光子灭绝.
- 从覆盖450至1600公里的高度的光谱数据推断出大气的特性.
主要成果:
- 鉴定并测量了六种物种:甲,乙,乙烯,乙,二乙烯和化.
- 在615公里处检测到一个中断期,最低温度为114K.
- 在大气层顶部确定了151K的非对称运动温度.
- 观察到较重的碳化合物和化在600-750公里以下急剧下降,甲在600公里以下占主导地位.
结论:
- 泰坦的上层大气表现出一个独特的分层结构与一个中断期.
- 甲是观察到的上层大气中较低区域中占主导地位的碳化合物分子.
- 丰富度资料为泰坦的大气模型提供了关键数据.
相关概念视频
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