Models of Haze on Saturn, Titan and Jupiter

土星、土卫六和木星上的雾霾模型

• 批准号: 9020730
• 负责人: Martin Tomasko
• 金额: $ 10.2万
• 依托单位: University of Arizona
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 1991
• 资助国家: 美国
• 起止时间: 1991-08-01 至 1995-07-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9020730&HistoricalAwards=false
• 关键词: Models; Haze; Saturn; Titan; Jupiter

Drs. Tomasko, Doose, and Peter Smith, at the University of Arizona, will analyze observations in hand and to be taken of Saturn, Titan, and Jupiter in a coordinated effort which makes use of several existing and new theoretical tools. These include: 1) input from photochemical calculations regarding the vertical profile of the production rates of gases that can form solid aerosol material; 2) extension of an existing cloud physics program that includes sedimentation, coagulation, and condensation to evaluate the number densities and size distribution of haze particles; 3) evaluation of the absorption coefficients of methane at low temperatures; 4) creation of a radiative transfer code for use in the thermal infrared; and 5) the use of radiative transfer modelling codes for evaluating the reflection and absorption of sunlight from an atmosphere containing the vertical distribution of haze predicted by the photochemical and cloud physics program. The bright and dark cloud features which dominate the appearance of Jupiter and Saturn play important roles in the chemistry, heat balance, and dynamics of their atmospheres. It is now known that a haze of small particles is formed in the stratospheres of Jupiter, Saturn, and Titan by photochemical reactions. These particles fall to tropospheric levels where they can act as nuclei for the condensation of several atmospheric gases such as ammonia and methane. The coordinated efforts of these investigators will greatly increase our understanding of the physical and chemical processes involved in the production, transport, and recycling of atmospheric aerosols as well as their role in driving the radiative and dynamical state of these atmospheres.

亚利桑那大学的托马斯科、杜斯和彼得·史密斯博士， 将分析对土星，土卫六， 和木星的协调努力，利用几个 现有和新的理论工具。 其中包括：（1）输入 光化学计算的垂直廓线 可形成固体气溶胶材料的气体的产生速率; 2） 现有云物理学计划的扩展，包括 沉淀、凝结和冷凝，以评估 混浊颗粒的密度和尺寸分布; 3）评价 甲烷在低温下的吸收系数; 4） 建立一个辐射传递代码，用于热 红外线;和5）使用辐射传输建模代码， 评估太阳光的反射和吸收 预测烟霾的垂直分布 由光化学和云物理计划。 明亮和黑暗的云特征主导了外观 在木星和土星的化学、热量、 大气层的平衡和动态。 现在已知 小颗粒的薄雾形成于 木星土星和土卫六的光化学反应。 这些 粒子落到对流层，在那里它们可以充当原子核 用于冷凝几种大气气体 和甲烷。 这些调查人员的协调努力将 大大提高了我们对物理和化学的理解 涉及生产、运输和回收的过程 大气气溶胶及其在驱动辐射 以及这些大气层的动态。