本文選題：嫦娥二號 + 4179小行星��； 參考：《哈爾濱工業(yè)大學(xué)》2015年碩士論文

【摘要】：在嫦娥二號飛越4179圖塔蒂斯小行星之前,人們對于它的了解和觀測主要是基于地基雷達(dá)的觀測。2012年12月13日嫦娥二號飛越圖塔蒂斯小行星,這是人類第一次近距離通過光學(xué)設(shè)備直接觀測近地小行星,并獲取了清晰的圖塔蒂斯小行星的清晰的可見光圖像。在1992年和1996年4179小行星近距離飛越地球時,天文學(xué)家們積累了大量地基雷達(dá)觀測數(shù)據(jù),從而推導(dǎo)出小行星的詳細(xì)形狀模型,本文中將此模型稱作圖塔蒂斯小行星的雷達(dá)模型�？梢姽鈭D像上圖塔蒂斯小行星的表面細(xì)節(jié)信息十分豐富,這些表面信息可以用來增強(qiáng)圖塔蒂斯小行星的雷達(dá)模型的表面結(jié)構(gòu)。在此應(yīng)用背景下,本文提出了一種使用嫦娥二號得到的圖塔蒂斯小行星的可見光圖像來修正其三維雷達(dá)模型的方法。文中首先仿真生成了不同光照角度與旋轉(zhuǎn)相位的雷達(dá)圖像,接著使用不變矩對生成的圖像和小行星可見光圖像進(jìn)行歸一化,讓小行星雷達(dá)圖像與可見光圖像具有相同的尺度與形心。然后通過鏈碼、邊界距離和不變矩的方法,對小行星雷達(dá)圖像和可見光圖像進(jìn)行了姿態(tài)定位,得到了兩組圖像的最佳擬合姿態(tài)。在此基礎(chǔ)上利用泰森多邊形建立了雷達(dá)模型上頂點(diǎn)和可見光圖像的像素之間的對應(yīng)關(guān)系。其次,因為可見光圖像是二維圖像,而雷達(dá)模型是由三維空間上的點(diǎn)組成的。所以需要計算可見光圖像的第三維深度信息,本文選取了從明暗恢復(fù)形狀(Shape From Shading)方法來計算可見光圖像的深度信息。最后,本文采用了數(shù)據(jù)融合的方法將可見光圖像深度信息代表表面細(xì)節(jié)的部分加載到了雷達(dá)模型上。頻率域中高頻信息代表表面結(jié)構(gòu)的細(xì)節(jié)信息,而低頻信息代表表面結(jié)構(gòu)的輪廓信息�？梢姽鈭D像上表面結(jié)構(gòu)的細(xì)節(jié)信息十分豐富,本文利用這種思想在頻率域中將雷達(dá)模型的深度的頻率域信息和通過高通濾波器的可見光圖像深度信息,最終得出了有更豐富的表面信息的雷達(dá)模型。
[Abstract]:Before Chang 'e-2 flew over the 4179 Tutatisse asteroid, people's understanding and observation of it was mainly based on ground-based radar observations. On December 13, 2012, Chang 'e-2 flew over the Tutatis asteroid, This is the first time that the near Earth asteroid has been observed directly by optical equipment and a clear visible light image of the Tutatisse asteroid has been obtained. In 1992 and 1996, when 4179 asteroid flew over the earth at close range, astronomers accumulated a large amount of ground-based radar observation data, thus deducing the detailed shape model of asteroid. This model is called the radar model of Tutatisse asteroid in this paper. The surface details of the Tatisse asteroid above the visible image are abundant and can be used to enhance the surface structure of the radar model of the Tuttis asteroid. In this context, this paper presents a method to correct the 3D radar model of the Tutatisse asteroid by using the visible light image of Chang 'e-2. In this paper, the radar images with different illumination angles and rotation phases are first simulated, and then the generated images and asteroid visible light images are normalized using invariant moments. Let the asteroid radar image and the visible image have the same scale and centroid. Then, the method of chain code, boundary distance and invariant moment is used to locate the attitude of asteroid radar image and visible light image, and the best fitting attitude of two groups of images is obtained. Based on this, the correspondence between vertices and pixels of visible image in radar model is established by using Tyson polygon. Secondly, because the visible image is a two-dimensional image, the radar model is composed of three-dimensional points. Therefore, it is necessary to calculate the third depth information of visible light image. In this paper, the shape from shading method is selected to calculate the depth information of visible light image. Finally, the method of data fusion is used to load the depth information of visible image to the radar model. The high frequency information in the frequency domain represents the detail information of the surface structure, while the low frequency information represents the contour information of the surface structure. The details of the surface structure on the visible light image are very rich. In this paper, the depth information of the radar model in frequency domain and the depth information of the visible light image through the high-pass filter are analyzed in the frequency domain. Finally, the radar model with more surface information is obtained.
【學(xué)位授予單位】：哈爾濱工業(yè)大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2015
【分類號】：P185.7

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相關(guān)期刊論文 前1條

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本文編號：2110811