本文選題：毛玻璃 + 太陽(yáng)望遠(yuǎn)鏡　； 參考：《科學(xué)通報(bào)》2017年26期

【摘要】：全日面太陽(yáng)光球像和色球像是監(jiān)測(cè)太陽(yáng)活動(dòng)的主要數(shù)據(jù),對(duì)望遠(yuǎn)鏡觀測(cè)的原始圖像進(jìn)行平場(chǎng)改正是數(shù)據(jù)處理過程中的基礎(chǔ)工作.本文嘗試?yán)妹Ａy(cè)量全日面太陽(yáng)光球和色球像的平場(chǎng),通過理論模擬和實(shí)地測(cè)量驗(yàn)證了該方法的有效性.首先,模擬計(jì)算了太陽(yáng)經(jīng)毛玻璃擴(kuò)散后在觀測(cè)視場(chǎng)內(nèi)形成的面光源的均勻性,其均勻度為99%,可以用來測(cè)量平場(chǎng).其次,在全日面太陽(yáng)光球和色球望遠(yuǎn)鏡上的實(shí)驗(yàn)結(jié)果表明,本方法獲得的平場(chǎng)像能夠改正原始觀測(cè)像中高頻的臟點(diǎn)和光路不均勻性,因平場(chǎng)觀測(cè)和常規(guī)觀測(cè)圖像中雜散光影響不同,導(dǎo)致平場(chǎng)改正像存在低頻失真,但可通過理論臨邊昏暗圖像對(duì)平場(chǎng)改正像進(jìn)行低頻信息修正.修正后的平場(chǎng)改正像與理論臨邊昏暗像相關(guān)系數(shù)達(dá)到0.99以上.最后,以HMI發(fā)布的光球像和GONG發(fā)布的色球像作為參考像,選取活動(dòng)區(qū)所在小視場(chǎng)和寧?kù)o區(qū)大視場(chǎng),分別與利用本方法實(shí)驗(yàn)改正后的光球像和色球像進(jìn)行了結(jié)構(gòu)相似度等方面的量化對(duì)比.對(duì)比結(jié)果表明,改正像的各項(xiàng)指標(biāo)均優(yōu)于原始像.本文提出的平場(chǎng)測(cè)量和改正方法簡(jiǎn)便易行,且容易實(shí)現(xiàn)自動(dòng)化測(cè)量,為全日面太陽(yáng)望遠(yuǎn)鏡的平場(chǎng)測(cè)量和改正提供了新方法.
[Abstract]:It is the basic work of data processing to correct the original image of the telescope for the correction of the flat field of the solar sphere image and color sphere image of the whole heliosphere to monitor the solar activity of the main data in the process of data processing. In this paper, we try to measure the flat field of sunballs and chromosphere images of all heliosphere by using ground glass. The effectiveness of this method is verified by theoretical simulation and field measurement. First, the uniformity of the surface light source formed in the observed field of view after the sun diffuses through the ground glass is simulated and calculated. The uniformity of the light source is 99%, which can be used to measure the flat field. Secondly, the experimental results on the sunball and color sphere telescope show that the flat-field image obtained by this method can correct the dirty points and the non-uniformity of the optical path in the original observation image. Because of the different influence of stray light in the plane field observation image and the conventional observation image, there is low frequency distortion in the flat field correction image, but the low frequency information of the level field correction image can be corrected by the theoretical edge dim image. The correlation coefficient between the corrected flat-field corrected image and the theoretical edge dim image is above 0.99. Finally, with the light sphere image published by HMI and the color sphere image published by long as reference images, the small field of view and the large field of view in quiet area are selected. The results are compared with the structure similarity of the optical spherical image and the color sphere image after the experimental correction by this method. The results show that the corrected image is superior to the original image. The flat field measurement and correction method presented in this paper is simple and easy to realize the automatic measurement, which provides a new method for the flat field measurement and correction of the solar telescope.
【作者單位】： 中國(guó)科學(xué)院國(guó)家空間科學(xué)中心;中國(guó)科學(xué)院大學(xué);中國(guó)科學(xué)院國(guó)家天文臺(tái);
【基金】：國(guó)家自然科學(xué)基金(11503063,11178005,11427901)資助
【分類號(hào)】：P182.2

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本文編號(hào)：2033973