摘要
火星是一个沙漠星球,沙尘的时空变化对火星气象和气候具有重要影响,例如大规模的沙尘暴活动会影响火星全球的大气结构和环流。火星的沙尘暴活动在时间上具有明显的季节性特征,主要分布在北半球秋冬季,即沙尘暴季节。在非全球性沙尘暴年份,沙尘暴季节内存在三次规律性的大型沙尘暴活动,按照发生的时间顺序可以标记为A、B、C类型,这3种类型的沙尘暴具有不同的持续时间、影响范围和强度。本研究利用第24到36火星年间火星柱积分的沙尘光学厚度数据(CDOD)对火星沙尘暴季节及不同类型的大型沙尘暴的年际变化情况进行了统计研究。研究发现,火星沙尘暴季节通常开始于太阳经度L_(S)=132°~156°左右,结束于次年L_(S)=5°~25°左右,持续时间在220°~240°之间波动,且沙尘暴季节的开始时间与结束时间存在一定的正相关,即开始时间早的年份,结束时间也较早;此外,A、B、C这3种类型的大型沙尘暴的发生时间、强度和影响范围存在年际变化规律,且A型和C型沙尘暴的开始时间和达到峰值时间之间存在一定的正相关,表明A型沙尘暴的发生时间可能会影响C型沙尘暴的发生时间。本研究还统计了第29到第36火星年间A、C型沙尘暴的起源位置,发现A型沙尘暴主要起源于中低纬度东经60°附近和西经60°附近,C型沙尘暴主要起源于中低纬度西经60°附近。这些发现为火星沙尘暴的预报和火星探测任务的安全性提供了重要参考。
As a desert planet,Mars exhibits significant atmospheric dust variability that critically influences its climatological and meteorological systems.Martian dust aerosols exert profound effects on atmospheric temperatures and dynamics,with particularly strong effects during regional and global dust storm events.Our analysis of column dust optical depth(CDOD)measurements from Martian Years(MY)24~36 reveals distinct seasonal patterns in dust storm activity,predominantly concentrated during the northern hemisphere autumn and winter-A period conventionally referred to as the‘dusty season’.In non-global dust storm years,three characteristic types of regional dust storms(classified as A,B,and C based on their temporal sequence)occur regularly within the dusty season,each with unique characteristics of duration,spatial extent,and intensity.Statistical analysis shows that the dusty season typically begins at solar longitude L_(S)=132°~156°and ends around L_(S)=5°~25°in the following Martian year,with the duration varying between 220°and 240°.In particular,we observe a positive correlation between the start and end of the season,with an earlier start consistently corresponding to an earlier end.Furthermore,our investigation of interannual variability shows that Type A and C storms exhibit significant temporal interdependence,with the initiation timing of Type A storms potentially influencing subsequent Type C events.Through systematic analysis of storm originating locations during MY 29~36,we identify that Type A storms predominantly originate near 60°E and 60°W at low-to-mid latitudes,while Type C storms primarily originate near 60°W within similar latitudinal bands.These findings provide an important reference for the forecasting of Martian dust storms and the safety of Mars exploration missions.
作者
何惠宁
吴兆朋
戎昭金
何飞
李勃
张江
王誉棋
高佳维
范开
魏勇
HE Huining;WU Zhaopeng;RONG Zhaojin;HE Fei;LI Bo;ZHANG Jiang;WANG Yuqi;GAO Jiawei;FAN Kai;WEI Yong(Key Laboratory of Planetary Science and Frontier Technology,Institute of Geology and Geophysics,Chinese Academy of Sciences,Beijing 100029,China;College of Earth and Planetary Science,University of Chinese Academy of Sciences,Beijing 100049,China;Institute of Space Sciences,Shandong University,Weihai 264209,China)
出处
《第四纪研究》
北大核心
2025年第4期882-893,共12页
Quaternary Sciences
基金
国家自然科学基金项目(批准号:42375119和42241135)
中国科学院重点部署项目(批准号:ZDBS-SSW-TLC00103)
中国科学院地质与地球物理研究所重点部署项目(批准号:IGGCAS-202102)
天问三号任务关键技术攻关项目(批准号:TW3006)共同资助。
关键词
火星大气
沙尘暴
时空分布
Martian atmosphere
dust storms
spatial and temporal distribution
