Haze formation on Pluto in the context of the solar cycle

冥王星的大气层在其范围内变化了十倍。PI提议调查冥王星大气层中的雾霾是否是由太阳活动周期引起的。研究小组将利用冥王星掩星的技术来探测冥王星大气层在太阳活动周期不同时刻的薄雾程度。（当行星或小天体，如冥王星，从星星前面经过时，就会发生掩星。）这颗星星的光不会立即消失，天文学家可以解释显示光衰减方式的精确数据来研究该天体？的大气层。该小组将使用小型便携式望远镜和数据采集系统来观测冥王星对明亮恒星的掩星。他们将争取业余天文学家和本科生的帮助，从而将许多非科学家引入STEM研究。雾霾形成过程的研究在几个方面都很重要。该小组将调查冥王星形成的分子清单？的大气层。霾的分布可能对冷却高层大气和抑制金斯逃逸有重要作用。通过结合FISM-P，Planet CARMA和KINETICS，该团队将执行三项关键任务：1）运行模型以量化冥王星的烟雾分布如何响应太阳紫外线通量的变化。此外，他们将使用模型来解决耀斑的问题（短期暴露于太阳能是否有效地转化为烟雾形成）和对太阳紫外线输出的非线性依赖性。2）比较模型与数据：模型产生的烟雾分布是否与来自20年恒星掩星时间跨度的烟雾光学深度的变化一致？3)测试冥王星的烟雾分布是否应随太阳通量而变化，然后预测明亮恒星掩星期间预期的烟雾分布。该奖项反映了NSF的法定使命，并通过使用基金会的知识价值和更广泛的影响审查标准进行评估，被认为值得支持。

Pluto's atmosphere varies in its extent by a factor of ten. The PI proposed to investigate whether, in particular, haze in Pluto's atmosphere is caused by the solar cycle. The team will use the techniques of stellar occultations by Pluto to probe the extent of Pluto's atmospheric haze at different points in the solar cycle. (Occultations occur when a planet or minor body, such as Pluto, passes in front of a star.) The star's light does not go away immediately, and astronomers can interpret precise data showing the way the light fades to study the object?s atmosphere. The team will use small portable telescopes and data acquisition systems to observe occultations of bright stars by Pluto. They will enlist the help of amateur astronomers and undergraduate students, thus introducing many non-scientists to STEM research.The study of haze formation processes is significant on several fronts. The team will investigate the inventory of molecules that form in Pluto?s atmosphere. Haze distributions may be important in cooling the upper atmosphere and inhibiting Jeans escape. By combining FISM-P, Planet CARMA and KINETICS, the team will perform three key tasks:1) Run models to quantify how Pluto's haze distribution responds to variations in solar UV flux. In addition, they will use the models to address the question of flares (does a short-term exposure to solar energy translate efficiently to haze formation) and non-linear dependencies on solar UV output.2) Compare model vs. data: do the models produce haze distributions that are consistent with the variation in haze optical depths derived from the 20-yr timespan of stellar occultations?3) Test whether Pluto's haze distribution should vary with solar flux, and then predictthe haze distribution that is expected during bright stellar occultations.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.