發(fā)布時(shí)間：2018-11-09 17:06

【摘要】：本文中通過(guò)分析火星勘測(cè)軌道飛行器(MRO)上搭載的火星氣候探測(cè)儀(MCS)2006～2013年(火星年28-31)的溫度觀測(cè)數(shù)據(jù),研究了火星中高層大氣的溫度和沙塵含量的季節(jié)變化。分析研究的結(jié)果表明：火星大氣中的溫度存在著明顯的季節(jié)變化,而且沙塵暴在火星大氣中是一個(gè)普遍存在的全球現(xiàn)象。論文的主要工作是對(duì)火星大氣中的緯向波數(shù)為s=1和2準(zhǔn)靜止行星波(QSPW)的季節(jié)變化和全球結(jié)構(gòu)特點(diǎn)等進(jìn)行了分析和研究。結(jié)果表明這兩支準(zhǔn)靜止行星波具有明顯的季節(jié)變化以及空間分布特征。準(zhǔn)靜止行星波主要出現(xiàn)在南北半球的中高緯度地區(qū),秋冬季節(jié)明顯增強(qiáng),而春夏季節(jié)相對(duì)較弱。對(duì)s＝1的準(zhǔn)靜止行星波的研究顯示：在冬季南半球s=1的準(zhǔn)靜止行星波明顯比冬季北半球波動(dòng)的振幅要強(qiáng),其中在南半球其振幅的極大值可以達(dá)到～12K,而在北半球這種波動(dòng)的最大振幅為～8K。另外在垂直方向上,波動(dòng)振幅的極大值主要位于100～10Pa和10～1Pa的兩個(gè)高度范圍內(nèi)。利用溫度的數(shù)據(jù),我們同時(shí)計(jì)算了位勢(shì)高度,位勢(shì)高度的極值位于溫度振幅兩個(gè)極大值區(qū)域的中間位置。此外對(duì)于s=2的準(zhǔn)靜止行星波的研究表明：s=2的準(zhǔn)靜止行星波的振幅明顯比s=1的波振幅弱,其最大振幅約為6K。 另外我們還利用火星氣候數(shù)據(jù)庫(kù)(MCD) version5.0的模擬結(jié)果與衛(wèi)星的觀測(cè)結(jié)果進(jìn)行了對(duì)比,結(jié)果表明模擬的結(jié)果與觀測(cè)是一致的,但模擬中得到的準(zhǔn)靜止行星波在南半球冬季存在的時(shí)間較短,此外,s=2的準(zhǔn)靜止行星波的振幅在北半球比觀測(cè)的結(jié)果要強(qiáng)很多。由此可見(jiàn),火星氣候數(shù)據(jù)庫(kù)為研究火星大氣氣候?qū)W提供了重要的參考,但對(duì)火星大氣動(dòng)力學(xué)過(guò)程的模擬有待進(jìn)一步的提高。此外我們還利用模式模擬了不同沙塵(多沙塵和少沙塵)條件下,s=1的準(zhǔn)靜止行星波的變化。模擬結(jié)果表明：在多沙塵環(huán)境中s=1準(zhǔn)靜止行星波的振幅比少沙塵環(huán)境中波的振幅要強(qiáng),這為我們研究沙塵與準(zhǔn)靜止行星波的變化關(guān)系提供了依據(jù),同時(shí)也有利于研究沙塵對(duì)火星氣候的影響。我們的結(jié)果為火星大氣模式的改進(jìn)提供了觀測(cè)依據(jù)。
[Abstract]:In this paper, the temperature data of Mars climate detector (MCS) 2006 ~ 2013 (Mars year 28-31) carried on the Mars Survey Orbiter (MRO) are analyzed, and the seasonal variations of temperature and dust content in the upper and middle atmosphere of Mars are studied. The results show that there are obvious seasonal variations in the temperature of the Martian atmosphere, and sandstorm is a universal phenomenon in the Martian atmosphere. The main work of this paper is to analyze and study the seasonal variation and global structural characteristics of the zonal wave number sz1 and 2 quasi stationary planetary wave (QSPW) in the atmosphere of Mars. The results show that the two quasi stationary planetary waves have obvious seasonal variation and spatial distribution. The quasi-stationary planetary waves mainly occur in the middle and high latitudes of the northern and southern hemispheres. The autumn and winter seasons are obviously strengthened, but the spring and summer seasons are relatively weak. The study on the quasi-stationary planetary wave of sf-1 shows that the amplitude of the quasi-stationary planetary wave in the southern hemisphere is obviously stronger than that in the northern hemisphere in winter, and the maximum amplitude of the amplitude in the southern hemisphere can reach ~ 12K. The maximum amplitude of this fluctuation in the Northern Hemisphere is ~ 8K. In addition, in the vertical direction, the maximum of wave amplitude lies in the two height ranges of 100~10Pa and 10~1Pa. Using the temperature data, we also calculate the potential height, the extreme value of the potential height is located in the middle of the two maximum regions of the temperature amplitude. In addition, the study on the quasi-stationary planetary wave of sf2 shows that the amplitude of the quasi stationary planetary wave of sf2 is obviously weaker than that of sf1, and its maximum amplitude is about 6K. In addition, the simulation results of Mars climate database (MCD) version5.0 are compared with the observed results of the satellite. The results show that the simulation results are consistent with the observations. However, the quasi-stationary planetary wave obtained in the simulation has a shorter duration in the southern hemisphere in winter. In addition, the amplitude of the quasi-stationary planetary wave of sf2 in the Northern Hemisphere is much stronger than that of the observational results in the Northern Hemisphere. It can be seen that the Martian climate database provides an important reference for the study of Martian atmospheric climatology, but the simulation of the Martian atmospheric dynamics needs to be further improved. In addition, we use the model to simulate the variation of quasi-stationary planetary wave of sf-1 under different conditions of sand dust (more sand dust and less sand dust). The simulation results show that the amplitude of sf-1 quasi stationary planetary wave is stronger than that in less sand dust environment, which provides a basis for us to study the relationship between sand dust and quasi stationary planetary wave. At the same time, it is helpful to study the influence of dust on the climate of Mars. Our results provide an observational basis for the improvement of the Martian atmospheric model.
【學(xué)位授予單位】：中國(guó)科學(xué)技術(shù)大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2014
【分類號(hào)】：P185.3

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相關(guān)期刊論文 前2條

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本文編號(hào)：2321042