【摘要】：太陽(yáng)系行星中,包含大氣的星球有地球、火星、木星、金星等。各行星具有不同的大氣成分和結(jié)構(gòu)。研究模擬行星大氣輻射傳輸過(guò)程對(duì)行星大氣成分探測(cè)、環(huán)境變化監(jiān)測(cè)等具有重要的意義。微波-亞毫米波是遙感行星大氣和表面的重要手段之一。常用的微波-亞毫米波大氣吸收模式MPM/PWR,只能得到水汽、氧氣、氮?dú)庠?-1000GHz頻段內(nèi)的吸收系數(shù),無(wú)法模擬其它氣體成分或更高頻率的吸收特性。針對(duì)探測(cè)地球中高層大氣成分或者其它行星大氣的需求,本文采用逐線(xiàn)積分方法,基于HIRTRAN數(shù)據(jù)庫(kù)中各氣體分子的光譜參數(shù),進(jìn)行各氣體分子在微波-亞毫米波波段吸收特征的模擬。利用輻射傳輸方程,對(duì)不同觀測(cè)方式下的行星大氣輻射亮溫進(jìn)行仿真,為后續(xù)地球乃至行星大氣成分探測(cè)模擬、頻帶的選擇以及大氣成分廓線(xiàn)反演提供模型及理論依據(jù)。本文首先詳述了地球及火星的大氣成分和結(jié)構(gòu)。闡述了向上觀測(cè)、垂直觀測(cè)以及臨邊觀測(cè)三種觀測(cè)方式的探測(cè)機(jī)理,并對(duì)常用微波亞毫米波大氣吸收模式MPM/PWR進(jìn)行分析。重點(diǎn)分析了國(guó)外的微波-亞毫米波大氣輻射傳輸模型的特點(diǎn)。之后,利用逐線(xiàn)積分方法計(jì)算行星大氣的氣體吸收系數(shù)。在逐線(xiàn)積分過(guò)程中,針對(duì)不同壓強(qiáng)溫度下的譜線(xiàn)線(xiàn)形的選擇進(jìn)行分析。為了在不影響精度的前提下提高計(jì)算速度,采用線(xiàn)形截?cái)嗟姆椒?并將逐線(xiàn)積分方法與MPM/PWR模式進(jìn)行了分析比較。通過(guò)計(jì)算行星大氣中各種氣體在特定溫度、壓強(qiáng)、密度下的1-3000GHz范圍內(nèi)的吸收系數(shù),分析了氣體在微波-亞毫米波波段的吸收特性,并定量分析了HIRTRAN2012數(shù)據(jù)庫(kù)中的譜線(xiàn)強(qiáng)度和空氣半展寬的不確定性帶來(lái)的系統(tǒng)誤差。最后,利用輻射傳輸方程,模擬了行星大氣輻射傳輸過(guò)程。進(jìn)行了向上觀測(cè)、天底觀測(cè)、臨邊觀測(cè)模式下的地球大氣輻射亮溫仿真;分析了地基微波-亞毫米波輻射計(jì)探測(cè)大氣污染物的可行性;進(jìn)行了臨邊探測(cè)下大氣成分變化的敏感性分析;根據(jù)火星大氣探測(cè)結(jié)果假設(shè)火星大氣廓線(xiàn)信息,仿真了臨邊探測(cè)下火星大氣的輻射亮溫。這些為進(jìn)一步行星大氣探測(cè)系統(tǒng)的通道設(shè)計(jì)和科學(xué)目標(biāo)獲取提供理論依據(jù)。
[Abstract]:Solar system planets, including the atmosphere of the planet Earth, Mars, Jupiter, Venus and so on. Each planet has different atmospheric composition and structure. It is of great significance to study the radiative transfer process of the planetary atmosphere to detect the composition of the planetary atmosphere and to monitor the environmental changes. Microwave-sub-millimeter wave is one of the important means of remote sensing planet atmosphere and surface. The microwave / submillimeter wave atmospheric absorption model MPM / PWR can only obtain the absorption coefficients of water vapor oxygen and nitrogen in the 1-1000GHz band and can not simulate the absorption characteristics of other gas components or higher frequencies. Aiming at the demand of detecting the upper atmosphere composition or other planetary atmospheres of the earth, the method of line by line integral is adopted in this paper, based on the spectral parameters of each gas molecule in the HIRTRAN database. The absorption characteristics of each gas molecule in microwave-submillimeter wave band were simulated. By using the radiation transfer equation, the radiative bright temperature of the planetary atmosphere under different observation modes is simulated, which provides a model and theoretical basis for the subsequent exploration simulation of the composition of the earth and the planetary atmosphere, the selection of the frequency band and the inversion of the atmospheric component profile. In this paper, the atmospheric composition and structure of Earth and Mars are described in detail. In this paper, the detection mechanism of upward observation, vertical observation and borderline observation is described, and the atmospheric absorption model MPM/PWR of microwave submillimeter wave is analyzed. The characteristics of microwave-submillimeter wave atmospheric radiation transfer model abroad are analyzed. After that, the gas absorption coefficient of the planetary atmosphere is calculated by the method of line-by-line integral. In the process of line-by-line integration, the selection of line shape at different pressure and temperature is analyzed. In order to improve the calculation speed without affecting the accuracy, the linear truncation method is adopted, and the line-by-line integral method is compared with the MPM/PWR model. By calculating the absorption coefficients of various gases in the planetary atmosphere in the range of 1-3000GHz at specific temperature, pressure and density, the absorption characteristics of gases in the microwave / submillimeter wave band are analyzed. The systematic error caused by the uncertainty of spectral line intensity and air half-broadening in HIRTRAN2012 database is analyzed quantitatively. Finally, the radiation transfer process of the planetary atmosphere is simulated by using the radiation transfer equation. The emulation of atmospheric radiation bright temperature in the mode of upward observation, bottom observation and observation at the edge of the earth is carried out, and the feasibility of detecting atmospheric pollutants by ground-based microwave and sub-millimeter wave radiometer is analyzed. The sensitivity analysis of atmospheric composition changes under the condition of edge detection is carried out, and the radiative brightness temperature of Mars atmosphere is simulated based on the assumption of Mars atmospheric profile information based on the results of Mars atmospheric exploration. These provide theoretical basis for the channel design and scientific target acquisition of further planetary atmospheric exploration system.
【學(xué)位授予單位】：中國(guó)科學(xué)院國(guó)家空間科學(xué)中心
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2016
【分類(lèi)號(hào)】：P185

【參考文獻(xiàn)】

相關(guān)期刊論文 前3條

1 史建魁;劉振興;程征偉;;火星探測(cè)研究結(jié)果分析[J];科技導(dǎo)報(bào);2011年10期

2 吳季;朱光武;趙華;王赤;李磊;孫越強(qiáng);郭偉;黃乘利;;螢火一號(hào)火星探測(cè)計(jì)劃的科學(xué)目標(biāo)[J];空間科學(xué)學(xué)報(bào);2009年05期

3 石廣玉;大氣輻射傳輸學(xué)[J];地球科學(xué)進(jìn)展;1991年05期

相關(guān)博士學(xué)位論文 前1條

1 郭晶;臨邊大氣背景光譜輻射特性研究[D];電子科技大學(xué);2015年

相關(guān)碩士學(xué)位論文 前1條

1 趙月鳳;微波臨邊探測(cè)儀系統(tǒng)研究與設(shè)計(jì)[D];中國(guó)科學(xué)院研究生院（空間科學(xué)與應(yīng)用研究中心）;2011年

，

本文編號(hào)：2173997