大視場日冕儀關(guān)鍵技術(shù)研究
發(fā)布時間：2019-04-23 12:33
【摘要】：日冕儀是觀測日冕和日冕物質(zhì)拋射現(xiàn)象的儀器。觀測日冕和日冕物質(zhì)拋射現(xiàn)象可以研究太陽磁場對地球的影響，并可以對影響地球及日地空間的災(zāi)害性空間天氣進行預(yù)警。本論文論及的大視場日冕儀是國際上首次設(shè)計的中心遮攔的大視場日冕儀，國際上報道的中心遮攔的日冕儀最大視場為30R⊙（R⊙為太陽半徑），大視場日冕儀在近地點的視場為72R⊙，在遠(yuǎn)地點的視場達到215R⊙，可以對太陽到地球范圍內(nèi)的日冕及日冕物質(zhì)拋射現(xiàn)象進行觀測。 本論文借鑒國際上日冕儀研制的經(jīng)驗，對日冕儀進行設(shè)計。本論文研制的大視場日冕儀光學(xué)系統(tǒng)主要參數(shù)為：視場為以太陽為中心±20度，像素分辨率為1.2arcmin，像素大小為13.5μm，波段為630nm～730nm，系統(tǒng)總長為896mm，其中光學(xué)系統(tǒng)總長為356mm，工作F數(shù)為5，像方焦距為40mm，傳遞函數(shù)大于0.65。 本論文研制的日冕儀由于視場遠(yuǎn)大于國際上現(xiàn)有的日冕儀，增加了日冕儀對雜散光抑制的要求。為此對日冕儀的雜散光抑制進行了深入研究。首先從理論上對日冕儀外掩體和外窗口的衍射雜散光水平進行了計算。其次，對大視場日冕儀的衍射雜散光和散射雜散光分別進行建模，，得到理論上雜散光的量級。衍射雜散光建模主要應(yīng)用分?jǐn)?shù)傅立葉變換理論和菲涅耳——基爾霍夫衍射積分理論，散射雜散光建模主要應(yīng)用ABC模型，對表面粗糙度和灰塵污染物造成的雜散光進行計算。最后，本文對大視場日冕儀所有可能產(chǎn)生的雜散光進行分級，并對其分別進行抑制。其中一級為太陽直射光；二級為外掩體和外窗口的衍射光；三級為物鏡口徑的衍射光，物鏡表面粗糙度和灰塵造成的散射光，拒熱鏡表面散射的雜散光和物鏡表面多次反射造成雜散光。最后對日冕儀整機雜散光進行檢測，總雜散光抑制水平達到10-11B⊙量級（B⊙為太陽平均亮度）。
[Abstract]:Corona is an instrument for observing coronal and coronal mass ejections. Observation of coronal and coronal mass ejections can be used to study the influence of solar magnetic field on the earth and early warning of disastrous space weather affecting the earth and solar-terrestrial space. The large-field coronation instrument discussed in this paper is the first designed in the world, and the maximum field of view of the center-occluded coronation instrument reported by the international report is 30R? The coronal and coronal mass ejections from the sun to the earth can be observed at the perigee and apogee by the large field of view coronograph (72R) and the apogee (215R). The coronal and coronal mass ejections from the sun to the earth can be observed in the range of the sun to the earth. This paper draws lessons from the experience of international coronal instrument development, and designs the coronal instrument. The main parameters of the optical system developed in this paper are as follows: the field of view is at the center of the sun 鹵20 degrees, the pixel resolution is 1.2 arcmin, the pixel size is 13.5 渭 m, the band is 630nm and 730nm, and the total length of the system is 896mm. The optical system has a total length of 356 mm, a working F number of 5, a square focal length of 40 mm and a transfer function of more than 0.65. Since the field of view of the coronal instrument developed in this paper is much larger than that of the existing coronal instrument in the world, the requirements of the coronal instrument for the suppression of stray light are increased. In this paper, the stray light suppression of the corona instrument is deeply studied. Firstly, the diffractive stray light level of the corona's outer bunker and outer window is calculated theoretically. Secondly, the diffractive stray light and scattered stray light of the large field corona instrument are modeled, and the order of stray light is obtained theoretically. The fractional Fourier transform theory and Fresnel-Kirchhoff diffraction integral theory are used in the modeling of diffracted stray light. The ABC model is mainly used to calculate the surface roughness and stray light caused by dust contaminants. Finally, in this paper, all possible stray light generated by the large field corona meter is graded, and the stray light is suppressed separately. The first is the direct solar light, the second is the diffracted light of the outer bunker and the outer window. The third order is the diffracted light of the aperture of the objective lens, the scattered light caused by the roughness of the surface of the objective lens and dust, the stray light scattered from the surface of the heat repellent lens and the spurious light caused by the reflection of the surface of the objective lens many times. Finally, the stray light of the corona instrument is detected, and the total stray light suppression level reaches the order of 10? 11B?
【學(xué)位授予單位】：中國科學(xué)院研究生院(長春光學(xué)精密機械與物理研究所)
【學(xué)位級別】：博士
【學(xué)位授予年份】：2014
【分類號】：TH753.12
本文編號：2463471
[Abstract]:Corona is an instrument for observing coronal and coronal mass ejections. Observation of coronal and coronal mass ejections can be used to study the influence of solar magnetic field on the earth and early warning of disastrous space weather affecting the earth and solar-terrestrial space. The large-field coronation instrument discussed in this paper is the first designed in the world, and the maximum field of view of the center-occluded coronation instrument reported by the international report is 30R? The coronal and coronal mass ejections from the sun to the earth can be observed at the perigee and apogee by the large field of view coronograph (72R) and the apogee (215R). The coronal and coronal mass ejections from the sun to the earth can be observed in the range of the sun to the earth. This paper draws lessons from the experience of international coronal instrument development, and designs the coronal instrument. The main parameters of the optical system developed in this paper are as follows: the field of view is at the center of the sun 鹵20 degrees, the pixel resolution is 1.2 arcmin, the pixel size is 13.5 渭 m, the band is 630nm and 730nm, and the total length of the system is 896mm. The optical system has a total length of 356 mm, a working F number of 5, a square focal length of 40 mm and a transfer function of more than 0.65. Since the field of view of the coronal instrument developed in this paper is much larger than that of the existing coronal instrument in the world, the requirements of the coronal instrument for the suppression of stray light are increased. In this paper, the stray light suppression of the corona instrument is deeply studied. Firstly, the diffractive stray light level of the corona's outer bunker and outer window is calculated theoretically. Secondly, the diffractive stray light and scattered stray light of the large field corona instrument are modeled, and the order of stray light is obtained theoretically. The fractional Fourier transform theory and Fresnel-Kirchhoff diffraction integral theory are used in the modeling of diffracted stray light. The ABC model is mainly used to calculate the surface roughness and stray light caused by dust contaminants. Finally, in this paper, all possible stray light generated by the large field corona meter is graded, and the stray light is suppressed separately. The first is the direct solar light, the second is the diffracted light of the outer bunker and the outer window. The third order is the diffracted light of the aperture of the objective lens, the scattered light caused by the roughness of the surface of the objective lens and dust, the stray light scattered from the surface of the heat repellent lens and the spurious light caused by the reflection of the surface of the objective lens many times. Finally, the stray light of the corona instrument is detected, and the total stray light suppression level reaches the order of 10? 11B?
【學(xué)位授予單位】：中國科學(xué)院研究生院(長春光學(xué)精密機械與物理研究所)
【學(xué)位級別】：博士
【學(xué)位授予年份】：2014
【分類號】：TH753.12
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