火星沙尘暴监测方法  

Monitoring methods for Martian dust storms

作　　者：何飞 魏勇[1,2] 戎昭金 任志鹏[1,2] 闫丽梅 谭宁[3] 王誉棋 范开 周旭 高佳维 Fei He;Yong Wei;Zhaojin Rong;Zhipeng Ren;Limei Yan;Ning Tan;Yuqi Wang;Kai Fan;Xu Zhou;Jiawei Gao(Key Laboratory of Earth and Planetary Physics,Institute of Geology and Geophysics,Chinese Academy of Sciences,Beijing 100029,China;College of Earth and Planetary Sciences,University of Chinese Academy of Sciences,Beijing 100049,China;Key Laboratory of Cenozoic Geology and Environment,Institute of Geology and Geophysics,Chinese Academy of Sciences,Beijing 100029,China)

机构地区：[1]中国科学院地质与地球物理研究所,中国科学院地球与行星物理重点实验室,北京100029 [2]中国科学院大学地球与行星科学学院,北京100049 [3]中国科学院地质与地球物理研究所,中国科学院新生代地质与环境重点实验室,北京100029

出　　处：《科学通报》2023年第16期2046-2057,共12页Chinese Science Bulletin

基　　金：国家自然科学基金(42222408,41922031);中国科学院重点部署项目(ZDBS-SSW-TLC00103);中国科学院地质与地球物理研究所重点部署项目(IGGCAS-201904,IGGCAS-202102);中国科学院青年创新促进会(Y2021027)资助。

摘　　要：沙尘暴是火星表面-大气-空间构成的圈层耦合系统中一种重要的天气现象.火星沙尘暴具有显著的季节性,但对不同时空尺度和等级的沙尘暴的发生规律至今仍认识不清.沙尘暴会对火星表面探测器带来诸多影响,如降低太阳能电池板发电量、降低环境温度、扰动大气密度和风场、阻碍通信、污染仪器等,是火星表面探测任务面临的最大安全威胁之一.本文系统性地回顾了人类历史上对火星沙尘暴的监测方法及其数据反演方法,以期为我国构建完善的火星沙尘暴监测体系提供基本的方法支撑.为了更好地保障和服务我国未来火星采样返回任务和后续火星探测任务,我国应考虑尽早建立完善的火星沙尘暴监测体系,这一体系应包含的探测方法包括着陆器可见光相机监测、环绕器可见-红外多光谱相机监测和地基光学望远镜监测.通过这些不同平台、不同时空尺度的监测手段相互配合,既能有效保障我国的火星探测任务安全实施,也将极大促进我国的火星系统科学研究.Dust storms are the most prominent weather processes in Martian physical system,involving the surface,atmosphere,and space environments.Martian dust storms possess significant seasonality,but how dust storms occur,with different spatiotemporal scales and strengths,remains a mystery to the academic community.Martian dust storms can be classified according to either their spatial or temporal scales.For the spatial methods,dust storms can be categorized as local,regional,and global dust storms.Several local dust storms can combine to produce regional dust storms,several of which can develop into a planet-encircling global dust storm.In terms of seasonality and the temporal scale,dust storms can be classified into Types A,B and C.Type A dust storms are planet encircling Southern Hemisphere events in spring and summer.Type B dust storms are southern polar events that occur around the summer solstice.Type C dust storms start well after the end of Type B storms in the middle-and low-latitude regions.Dust storms are quantitatively evaluated using the parameter of the column integrated dust optical depth(DOD),which denotes how much of the radiation at a specific wavelength(from visible to infrared)would be absorbed or scattered by the airborne dust particles.The larger the DOD,the stronger the dust storm.The effective radii of the dust particles usually vary from~0.5 to 2μm during the dust season and are proportional to the DOD.However,during large global dust storms,the dust particle effective radius can increase to 4μm or greater when the visible-light DOD exceeds 6.Dust storms greatly impact landers/rovers and sample return missions on the Martian surface by disturbing the atmospheric density and wind,threatening the safety of the entry-descent-landing system,degrading the efficiency of the solar cells due to both dust cover and obstructing the incident solar radiation,decreasing the environmental temperature and thermal control,blocking telecommunications,and polluting the instruments.For example,the Opportunity rov

关 键 词：火星沙尘暴 监测 光学厚度 可见光 红外 望远镜 

分 类 号：P185.3[天文地球—天文学]