火星大气中准静止行星波的分析研究
发布时间：2018-11-09 17:06
【摘要】：本文中通过分析火星勘测轨道飞行器(MRO)上搭载的火星气候探测仪(MCS)2006～2013年(火星年28-31)的温度观测数据,研究了火星中高层大气的温度和沙尘含量的季节变化。分析研究的结果表明：火星大气中的温度存在着明显的季节变化,而且沙尘暴在火星大气中是一个普遍存在的全球现象。论文的主要工作是对火星大气中的纬向波数为s=1和2准静止行星波(QSPW)的季节变化和全球结构特点等进行了分析和研究。结果表明这两支准静止行星波具有明显的季节变化以及空间分布特征。准静止行星波主要出现在南北半球的中高纬度地区,秋冬季节明显增强,而春夏季节相对较弱。对s＝1的准静止行星波的研究显示：在冬季南半球s=1的准静止行星波明显比冬季北半球波动的振幅要强,其中在南半球其振幅的极大值可以达到～12K,而在北半球这种波动的最大振幅为～8K。另外在垂直方向上,波动振幅的极大值主要位于100～10Pa和10～1Pa的两个高度范围内。利用温度的数据,我们同时计算了位势高度,位势高度的极值位于温度振幅两个极大值区域的中间位置。此外对于s=2的准静止行星波的研究表明：s=2的准静止行星波的振幅明显比s=1的波振幅弱,其最大振幅约为6K。 另外我们还利用火星气候数据库(MCD) version5.0的模拟结果与卫星的观测结果进行了对比,结果表明模拟的结果与观测是一致的,但模拟中得到的准静止行星波在南半球冬季存在的时间较短,此外,s=2的准静止行星波的振幅在北半球比观测的结果要强很多。由此可见,火星气候数据库为研究火星大气气候学提供了重要的参考,但对火星大气动力学过程的模拟有待进一步的提高。此外我们还利用模式模拟了不同沙尘(多沙尘和少沙尘)条件下,s=1的准静止行星波的变化。模拟结果表明：在多沙尘环境中s=1准静止行星波的振幅比少沙尘环境中波的振幅要强,这为我们研究沙尘与准静止行星波的变化关系提供了依据,同时也有利于研究沙尘对火星气候的影响。我们的结果为火星大气模式的改进提供了观测依据。
[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.
【学位授予单位】：中国科学技术大学
【学位级别】：硕士
【学位授予年份】：2014
【分类号】：P185.3
本文编号：2321042
[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.
【学位授予单位】：中国科学技术大学
【学位级别】：硕士
【学位授予年份】：2014
【分类号】：P185.3
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相关期刊论文 前2条
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