本文關(guān)鍵詞：月球表面FeO豐度反演與火星大氣沙塵懸浮層數(shù)值模擬研究　出處：《華東師范大學》2016年博士論文　論文類型：學位論文

  更多相關(guān)文章： 月球 IIM FeO 火星 沙塵 懸浮層 火箭沙塵暴 坡度風

【摘要】：隨著深空探測戰(zhàn)略的穩(wěn)步推進,月球和火星已成為我國空間探測的重要研究對象。同時近期發(fā)布的《國土資源“十三五”科技創(chuàng)新發(fā)展規(guī)劃》中提出,積極推進行星地質(zhì)研究,開展火星和月球試驗場建設(shè)研究、“地-月-火星”對比研究；組織月球與火星地質(zhì)編圖等內(nèi)容。這將進一步推進我國深空探測與行星科學的發(fā)展。我國第一顆自主繞月衛(wèi)星嫦娥一號搭載的干涉成像光譜儀(Interference Imaging Spectrometer, IIM)獲取了大量月球高光譜數(shù)據(jù)。雖然已有研究對ⅡM數(shù)據(jù)開展了數(shù)據(jù)處理和應(yīng)用研究,但ⅡM數(shù)據(jù)預處理過程仍存在問題,主要有壞點噪聲未能得到較好地去除,利用月壤樣品定標的反射率產(chǎn)品與月球表面實際情況相差較大,交叉定標過程采用的參考地基望遠鏡數(shù)據(jù)過少,不足以代表月球表面復雜多樣的地物類型,處理后的ⅡM反射率數(shù)據(jù)在拼接過程中邊界明顯,光度均一性差。沙塵是火星大氣氣溶膠重要組成部分,其空間分布影響著火星大氣的熱力平衡。搭載于Mars Reconnaissance Orbiter上的Mars Climate Sounder (MCS)發(fā)現(xiàn)了火星沙塵在大氣行星邊界層之上存在明顯的懸浮特征。在春夏季,該懸浮層夜間高度維持在約20km高空處；在秋冬季,懸浮層夜間高度變化較為劇烈,變化幅度可達20km。MCS觀測發(fā)現(xiàn)的火星大氣沙塵懸浮層在之前的觀測和研究中均未被發(fā)現(xiàn),這一大尺度廣泛存在的懸浮層形成機制尚不清楚。針對上述內(nèi)容,本論文開展了相關(guān)的科學研究,并取得一定進展與突破。主要研究結(jié)果與結(jié)論如下：(1)為了去除ⅡM數(shù)據(jù)中壞點噪聲,本文提出了一種基于光譜角和歐式距離的壞點檢測與修正算法,經(jīng)過目視和與其它研究對比分析發(fā)現(xiàn),新方法可以較好地去除ⅡM數(shù)據(jù)中的壞點,壞點識別準確,誤判率低；為了改進ⅡM反射率定標,本文提出一種新的ⅡM數(shù)據(jù)在軌定標方式,通過建立四類光度模型對ⅡM數(shù)據(jù)進行光度校正,獲得月表真實反射率產(chǎn)品,研究結(jié)果表明新的ⅡM反射率產(chǎn)品光度均一性得到顯著改善,相鄰影像邊界問題被很好地去除,同時擺脫了以月壤樣品反射率為參考的定標方法導致的ⅡM反射率過高問題；本文還通過引入更多精度較高、代表地物類型更多的地基望遠鏡數(shù)據(jù)進行ⅡM高光譜數(shù)據(jù)交叉定標研究以修正ⅡM數(shù)據(jù)在近紅外波段反射率過低的問題。(2)本文對經(jīng)過預處理的ⅡM數(shù)據(jù)開展了FeO反演最優(yōu)波段選擇的研究,通過設(shè)置對比實驗,研究發(fā)現(xiàn)對于ⅡM數(shù)據(jù)來說,經(jīng)過交叉定標的891 nm波段是最適合月球FeO反演的近紅外波段；基于此,本文利用ⅡM數(shù)據(jù)反演了全月FeO豐度,研究結(jié)果發(fā)現(xiàn)本文反演結(jié)果與Clementine反演結(jié)果整體趨勢一致,月海FeO豐度較高,高地較低,本文反演的FeO豐度在月海地區(qū)比Clementine反演FeO豐度略低,在高地地區(qū)比Clementine反演結(jié)果略高。(3)為了能夠在GCM中模擬MCS觀測的火星大氣沙塵懸浮層,本文在LMDMars GCM中設(shè)計并實施了“火箭”沙塵暴物理參數(shù)化過程,研究結(jié)果表明,在火星秋冬季節(jié),在添加“火箭”沙塵暴物理參數(shù)化后,GCM具備了模擬沙塵懸浮層的能力,且模式模擬的沙塵懸浮層的形成和演化均與MCS觀測相吻合；研究結(jié)果還發(fā)現(xiàn)沙塵暴對流導致懸浮層高度在垂直方向上劇烈變化,該變化與觀測相符。因此,在全球尺度上,“火箭”沙塵暴是火星秋冬季沙塵懸浮層形成機制之一；研究結(jié)果還發(fā)現(xiàn),僅考慮“火箭”沙塵暴過程,模式無法模擬出火星春夏季沙塵懸浮層結(jié)構(gòu)；(4)為繼續(xù)探究火星大氣沙塵懸浮層在春夏季形成原因,本文在LMD MarsGCM中設(shè)計并實施了日間坡度風效應(yīng)物理參數(shù)化過程,研究結(jié)果表明,在日間坡度風的作用下,GCM可以重現(xiàn)春夏季沙塵懸浮層結(jié)構(gòu),模式模擬的懸浮層高度和變化趨勢與MCS觀測具有可比性,因此說明坡度風是春夏季MCS觀測的大氣沙塵懸浮層的主要形成原因。模擬發(fā)現(xiàn)坡度風作用下形成的沙塵懸浮層高度在垂直方向上變化小,說明坡度風產(chǎn)生的對流比“火箭”沙塵暴產(chǎn)生的對流要弱。
[Abstract]:With the steady progress of deep space exploration strategy, the moon and Mars has become an important research object in space exploration. At the same time, the recent release of the "land resources" in 13th Five-Year "the innovation of science and technology development plan > proposed to actively promote the development of planetary geology, Mars and the moon test field construction research," research "- month - contrast the moon and Mars Mars; organization of geological mapping and so on. This will further promote the development of deep space exploration and planetary science. China's first independent lunar satellite Chang'e interference imaging spectrometer, equipped with (Interference Imaging Spectrometer, IIM) to obtain a large number of lunar hyperspectral data. Although research has carried out data study on the processing and application of M II M II data, but the data pretreatment process is still a problem, the main point has not been effectively remove noise, calibration using the regolith sample counter The surface of the moon at a rate of products and the difference among the actual situation, cross reference calibration process using ground-based telescope data is too small, not enough to represent the feature type of the lunar surface complex, II M reflectivity data after a sharp boundary in the splicing process, photometric uniformity. Dust aerosol is an important part of Mars, the space the distribution affects the thermodynamic equilibrium of the Martian atmosphere. Mars Reconnaissance Orbiter equipped with Mars Climate Sounder (MCS) found in the atmosphere of Mars dust on the planetary boundary layer has obvious suspension characteristics. In spring and summer, the suspension layer remained at about 20km at night high altitude; in the autumn and winter, the suspension layer height change at night the more violent, the atmosphere of Mars dust suspension layer change rate of up to 20km.MCS observation found in previous studies and observations have not been found, a large scale wide The suspension layer ubiquitous formation mechanism is not clear. In view of the above content, this paper carried out the relevant scientific research, and have made certain progress and breakthrough. The main research results and conclusions are as follows: (1) in order to remove the noise of dead M data, this paper proposes a fault detection and correction algorithm for angle and Euclidean distance the optical spectrum based on the visual and other research results, the new method can effectively remove dead II M data, defect recognition accuracy, low misjudgment rate; in order to improve the calibration of reflectivity of M, this paper proposes a new M data on orbit calibration methods, through the establishment of four kinds of photometric model on the M data obtained from photometric calibration, the true reflectance products, the results of the study show that M photometric uniformity of new reflectivity products has been significantly improved, the adjacent image boundary problem is well removed, while getting rid of the In the lunar soil samples reflectance calibration method of the reference to the problem of high reflectivity M II; through the introduction of more precision, more representative types of telescope data of M hyperspectral data cross calibration study to correct the problem in the near infrared reflectance of low M data (2) in this paper. After M data preprocessing to carry out research on selection of FeO inversion optimal bands, by setting the contrast experiment, the study found that M data, after 891 nm band cross calibration is the most suitable for the near infrared band of FeO inversion; based on this, this paper uses M data inversion of the whole month of FeO abundance the results showed that this inversion results and Clementine results overall trend, Maria FeO high abundance, high low FeO abundance in the sea area than the Clementine inversion inversion of FeO abundance slightly Low in upland regions. The results of Clementine inversion is slightly higher (3) in order to simulate the Mars atmospheric dust suspension layer observed by MCS in GCM, this paper designed and implemented the "physical parameters of rocket" Sandstorm Process in LMDMars GCM, the results of the study show that, in the autumn and winter festival on Mars, "added physical parameters the rocket" sandstorm after, GCM has the ability to simulate dust suspension layer, and the formation of dust suspension layer in the model simulation and evolution are consistent with MCS observations; the research results also show that the sandstorm convection causes dramatic changes in suspension height in the vertical direction, consistent with the change and observation. Therefore, in the global scale on the "rocket" sandstorm is Mars in autumn and winter dust formation mechanism of the suspension layer; the study also found that only consider the "rocket" Sandstorm Process Model to simulate Martian spring and summer dust suspension layer structure; (4) to continue to explore Mars atmospheric dust suspension layer in the spring and summer causes, this paper design and implement the daytime slope wind effect physical parameters in the process of LMD MarsGCM, the results show that the slope under the action of wind in the daytime, GCM can reproduce in spring and summer dust suspension layer structure model to simulate the suspension height and the changing trend and MCS observations are comparable, so that the slope wind is the main causes of spring and summer MCS observations of atmospheric dust suspended layer. Simulation shows that dust suspension layer is formed under the action of gradient wind height in the vertical direction change is small, that convection generated by wind slope than the "rocket" sandstorm to be weak.

【學位授予單位】：華東師范大學
【學位級別】：博士
【學位授予年份】：2016
【分類號】：P184;P185.3

【參考文獻】

相關(guān)期刊論文 前10條

1 凌宗成;張江;劉建忠;李勃;武中臣;倪宇恒;孫靈芝;陳劍;;嫦娥一號干涉成像光譜儀數(shù)據(jù)再校正與全月鐵鈦元素反演[J];巖石學報;2016年01期

2 張霞;帥通;趙冬;;干涉成像光譜儀高光譜數(shù)據(jù)信息質(zhì)量評估[J];紅外與毫米波學報;2012年02期

3 歐陽自遠;肖福根;;火星探測的主要科學問題[J];航天器環(huán)境工程;2011年03期

4 凌宗成;張江;劉建忠;張文喜;張廣良;劉斌;任鑫;牟伶俐;劉建軍;李春來;;嫦娥一號干涉成像光譜儀數(shù)據(jù)TiO_2反演初步結(jié)果[J];科學通報;2011年16期

5 ;Preliminary results of FeO mapping using Imaging Interferometer data from Chang'E-1[J];Chinese Science Bulletin;2011年Z1期

6 凌宗成;張江;劉建忠;張文喜;邊偉;任鑫;牟伶俐;劉建軍;李春來;;“嫦娥一號”干涉成像光譜儀數(shù)據(jù)FeO反演初步結(jié)果[J];科學通報;2010年35期

7 ;Estimation of lunar titanium content: Based on absorption features of Chang’E-1 interference imaging spectrometer (ⅡM)[J];Science China(Physics,Mechanics & Astronomy);2010年12期

8 趙葆常;楊建峰;薛彬;喬衛(wèi)東;邱躍洪;;嫦娥一號干涉成像光譜儀的定標[J];光子學報;2010年05期

9 歐陽自遠;李春來;鄒永廖;張洪波;呂昌;劉建忠;劉建軍;左維;蘇彥;溫衛(wèi)斌;邊偉;趙葆常;王建宇;楊建峰;常進;王煥玉;張曉輝;王世金;汪敏;任鑫;牟伶俐;孔德慶;王曉倩;王芳;耿良;張舟斌;鄭磊;朱新穎;鄭永春;李俊鐸;鄒小端;許春;施碩彪;高亦菲;高冠男;;繞月探測工程的初步科學成果[J];中國科學:地球科學;2010年03期

10 吳昀昭;徐夕生;謝志東;唐澤圣;;嫦娥一號IIM數(shù)據(jù)絕對定標與初步應(yīng)用[J];中國科學(G輯:物理學 力學 天文學);2009年10期

，

本文編號：1382524