白光日冕儀雜散光抑制的關(guān)鍵技術(shù)研究
發(fā)布時間：2019-01-08 12:49
【摘要】：日冕是太陽大氣的最外層,從色球邊緣向外延伸到幾個太陽半徑處,廣義上的日冕范圍甚至包括地球周圍的空間環(huán)境。劇烈的日冕活動(太陽風(fēng)、日冕物質(zhì)拋射等)嚴(yán)重影響日地空間環(huán)境。日冕儀是用于非日食情況下,對太陽日冕以及日冕拋射現(xiàn)象進(jìn)行實時觀測的光學(xué)儀器。本文以夸父計劃中白光日冕儀的技術(shù)指標(biāo)為基礎(chǔ),設(shè)計并完成了國內(nèi)首臺外掩式白光日冕儀原理演示樣機(jī)。以此原理演示樣機(jī)為基礎(chǔ),進(jìn)行了外掩式白光日冕儀雜散光抑制關(guān)鍵技術(shù)的研究。日冕儀原理演示樣機(jī)的主要參數(shù)如下:視場為±2.5-15 R⊙(R⊙表示一個太陽半徑,約為16’),口徑為30mm,有效焦距200mm,分辨率為14sec/pixel,工作波段為650-750nm。相比太陽光球?qū)拥牧炼?日冕光的亮度極其微弱,因此日冕儀雜散光抑制是日冕儀系統(tǒng)的關(guān)鍵問題。日冕儀雜散光根據(jù)形成機(jī)理不同行大致分為五類:太陽直射光;系統(tǒng)光孔的衍射光;物鏡表面二次反射光;透鏡加工精度所引起的雜散光;玻璃材料本身缺陷等引起的雜散光。本文首先對這五類雜散光產(chǎn)生的主要原因進(jìn)行理論分析,這里應(yīng)用分?jǐn)?shù)傅里葉變換理論分析了外掩體邊緣衍射光能量,并通過ASAP軟件建模分析了物鏡表面二次反射形成鬼像雜散光的機(jī)理。然后,論文中針對各級雜散光形成機(jī)理的不同,分別提出了相應(yīng)的抑制方法,使用Trace Pro軟件,針對拒熱鏡對太陽直射光的抑制,視場光闌對外窗口邊緣衍射光遮攔,以及內(nèi)掩體對外掩體邊緣衍射光的遮攔進(jìn)行了模擬分析。此外,論文還就外掩式日冕儀內(nèi)視場漸暈的問題進(jìn)行了理論分析和計算機(jī)模擬,得到了日冕儀漸暈隨視場變化的規(guī)律,并模擬出二維等暈圖。為了對日冕儀雜散光抑制有更深入的研究,根據(jù)理論部分提出的日冕儀雜散光分級抑制的方法,設(shè)計相對應(yīng)的實驗,觀測各級雜散光的抑制情況。實驗結(jié)果顯示日冕儀各級雜散光抑制的方法切實有效,雜散光得到了很好的抑制。最后,本文對外掩式日冕儀原理演示樣機(jī)雜散光抑制整體水平進(jìn)行檢測,總體雜散光抑制水平可以達(dá)到10-9 B⊙量級(其中B⊙代表太陽光球?qū)悠骄炼?。
[Abstract]:The corona is the outermost layer of the solar atmosphere, extending from the edge of the chromosphere to several solar radii. In a broad sense, the coronal range even includes the space environment around the earth. Intense coronal activity (solar wind, coronal mass ejection, etc.) seriously affects the solar-terrestrial space environment. Coronal apparatus is an optical instrument for real-time observation of the solar corona and its ejection in the case of non-solar eclipse. Based on the technical specifications of the white corona apparatus in the Kuafa project, the principle demonstration prototype of the first mask white corona apparatus in China has been designed and completed in this paper. Based on the principle demonstration prototype, the key technology of stray light suppression of the white coronal apparatus is studied. The main parameters of the prototype are as follows: the field of view is 鹵2.5-15R _ (-) (R _ denote a solar radius, about 16'), the aperture is 30 mm, the effective focal length is 200 mm, the resolution is 14 sec-p pixel, and the working band is 650-750 nm. Compared with the brightness of the solar photosphere, the brightness of the coronal light is very weak, so the suppression of stray light is the key problem in the coronal system. Coronal instrument stray light is divided into five categories according to its formation mechanism: direct solar light; diffraction light from the system aperture; secondary reflection light from the surface of the objective lens; stray light caused by the machining accuracy of the lens; and the stray light caused by the defects of the glass material itself. In this paper, the main causes of these five kinds of stray light are analyzed theoretically. Here, the energy of diffractive light at the edge of the outer mask is analyzed by using the fractional Fourier transform theory. The mechanism of the secondary reflection of the objective lens is analyzed by ASAP software. Then, aiming at the different formation mechanism of stray light at different levels, the corresponding suppression methods are put forward in this paper. By using Trace Pro software, aiming at the suppression of direct solar light by the thermal rejection mirror, the diffraction light of the external window of the field of view aperture is shaded. And the external mask edge diffractive light is simulated and analyzed. In addition, theoretical analysis and computer simulation are carried out on the camouflage of the camouflage in the coronal instrument. The variation of the camber with the field of view is obtained, and the 2-D isohalo pattern is simulated. In order to study the suppression of stray light in coronal instrument more deeply, according to the method of hierarchical suppression of stray light proposed in the theoretical part, a corresponding experiment was designed to observe the suppression of stray light at all levels. The experimental results show that the method of suppression of stray light at all levels of the coronal apparatus is effective and the stray light is well suppressed. Finally, the principle of the external mask coronal apparatus is used to demonstrate the whole level of stray light suppression of the prototype. The total stray light suppression level can reach 10 ~ (-9) B ~ (-) (where B _ (?) represents the average brightness of the solar photosphere).
【學(xué)位授予單位】：沈陽理工大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2015
【分類號】：P111.41
本文編號：2404622
[Abstract]:The corona is the outermost layer of the solar atmosphere, extending from the edge of the chromosphere to several solar radii. In a broad sense, the coronal range even includes the space environment around the earth. Intense coronal activity (solar wind, coronal mass ejection, etc.) seriously affects the solar-terrestrial space environment. Coronal apparatus is an optical instrument for real-time observation of the solar corona and its ejection in the case of non-solar eclipse. Based on the technical specifications of the white corona apparatus in the Kuafa project, the principle demonstration prototype of the first mask white corona apparatus in China has been designed and completed in this paper. Based on the principle demonstration prototype, the key technology of stray light suppression of the white coronal apparatus is studied. The main parameters of the prototype are as follows: the field of view is 鹵2.5-15R _ (-) (R _ denote a solar radius, about 16'), the aperture is 30 mm, the effective focal length is 200 mm, the resolution is 14 sec-p pixel, and the working band is 650-750 nm. Compared with the brightness of the solar photosphere, the brightness of the coronal light is very weak, so the suppression of stray light is the key problem in the coronal system. Coronal instrument stray light is divided into five categories according to its formation mechanism: direct solar light; diffraction light from the system aperture; secondary reflection light from the surface of the objective lens; stray light caused by the machining accuracy of the lens; and the stray light caused by the defects of the glass material itself. In this paper, the main causes of these five kinds of stray light are analyzed theoretically. Here, the energy of diffractive light at the edge of the outer mask is analyzed by using the fractional Fourier transform theory. The mechanism of the secondary reflection of the objective lens is analyzed by ASAP software. Then, aiming at the different formation mechanism of stray light at different levels, the corresponding suppression methods are put forward in this paper. By using Trace Pro software, aiming at the suppression of direct solar light by the thermal rejection mirror, the diffraction light of the external window of the field of view aperture is shaded. And the external mask edge diffractive light is simulated and analyzed. In addition, theoretical analysis and computer simulation are carried out on the camouflage of the camouflage in the coronal instrument. The variation of the camber with the field of view is obtained, and the 2-D isohalo pattern is simulated. In order to study the suppression of stray light in coronal instrument more deeply, according to the method of hierarchical suppression of stray light proposed in the theoretical part, a corresponding experiment was designed to observe the suppression of stray light at all levels. The experimental results show that the method of suppression of stray light at all levels of the coronal apparatus is effective and the stray light is well suppressed. Finally, the principle of the external mask coronal apparatus is used to demonstrate the whole level of stray light suppression of the prototype. The total stray light suppression level can reach 10 ~ (-9) B ~ (-) (where B _ (?) represents the average brightness of the solar photosphere).
【學(xué)位授予單位】：沈陽理工大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2015
【分類號】：P111.41
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，本文編號：2404622
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