本文選題：太陽大氣活動 + 太陽光柵光譜儀　； 參考：《電子科技大學(xué)》2016年博士論文

【摘要】：眾所周知,不息衍化的太陽磁場是導(dǎo)致太陽大氣活動爆發(fā)的根本原因,如太陽黑子,米粒和耀斑等。同時,激烈的太陽活動及周期變化,又影響和調(diào)制著人類的生存環(huán)境。因此,實(shí)時的監(jiān)視和預(yù)報太陽大氣活動具有重要意義。而成像型太陽光柵光譜儀是實(shí)現(xiàn)這一目標(biāo)的重要儀器。它不僅能夠?qū)μ柎髿饣顒舆M(jìn)行成像觀測。同時,又能根據(jù)獲得的光譜信息來確定爆發(fā)的太陽大氣活動的熱力學(xué)參數(shù),如磁場,溫度,壓強(qiáng)和元素豐度等。因此,太陽光柵光譜儀廣泛的用于太陽大氣活動的觀測。本文研究的高光譜分辨率的太陽光柵光譜儀包括以下四個部分內(nèi)容:高光譜分辨率太陽光柵光譜儀的設(shè)計(jì)、原理樣機(jī)的研制、波前像差對太陽光柵光譜儀性能參數(shù)的影響分析及實(shí)驗(yàn)驗(yàn)證。第一,對小型化高分辨率太陽光柵光譜儀進(jìn)行了深入的研究�；谙癫罾碚�,設(shè)計(jì)了一套基于一米紅外太陽望遠(yuǎn)鏡NVST的高光譜分辨率的光柵光譜儀,具有在656.3nm和854.2nm同時成像的能力。為了使光柵光譜儀具有良好的成像能力,本文對光柵光譜儀中的球差、彗差和象散進(jìn)行了補(bǔ)償。確定了系統(tǒng)的初始結(jié)構(gòu),并采用光學(xué)設(shè)計(jì)軟件ZEMAX進(jìn)行了優(yōu)化設(shè)計(jì)。設(shè)計(jì)結(jié)果表明,光柵光譜儀的成像能力達(dá)到了衍射極限。這對于精確的太陽大氣成像和精確的太陽大氣熱力學(xué)參數(shù)測量具有重要意義。第二,研制了高光譜分辨率太陽光柵光譜儀原理樣機(jī),從儀器設(shè)計(jì)、關(guān)鍵元件設(shè)計(jì)、白光光譜測量及波長定標(biāo)和原理樣機(jī)的光譜分辨率確定等多個方面,系統(tǒng)地介紹了高光譜分辨率太陽光柵光譜儀的研制方法和過程。為了降低光柵光譜儀裝調(diào)難度及更好的與太陽望遠(yuǎn)鏡系統(tǒng)對接,我們設(shè)計(jì)了一個的定標(biāo)光源系統(tǒng)。為了能夠更好的消除光柵光譜儀的系統(tǒng)像差,我們在光柵光譜儀的定標(biāo)光源系統(tǒng)中集成了自適應(yīng)光學(xué)系統(tǒng)。實(shí)驗(yàn)結(jié)果表明:研制的光譜儀器工作波長覆蓋范圍0.6μm~1.1μm;實(shí)際光譜分辨率為5.6pm@632.8nm,光譜分辨率指標(biāo)達(dá)到了世界同類光譜儀器水平。此外,太陽光柵光譜儀實(shí)際的空間分辨率為55μm,接近衍射極限的空間分辨率(50μm)。第三,深入分析了波前像差對高光譜分辨率太陽光柵光譜儀的光譜成像性能的影響。與一般光學(xué)不同,光譜儀中的狹縫較小,對波前像差具有一定程度的濾波作用。因此,對波前像差和光譜成像性能參數(shù)之間的數(shù)學(xué)關(guān)系進(jìn)行了理論推導(dǎo),并進(jìn)行了數(shù)值模擬仿真。結(jié)果表明:經(jīng)過狹縫濾波后,不同類型、不同大小的波前像差對光譜分辨率和能量利用率的影響不同,且與濾波前相比,波前像差對光譜分辨率和能量利用率的影響變小。狹縫越小,其濾波作用越強(qiáng)。但是,對于以低頻為主的像差如離焦像差而言,狹縫越小,其低頻也會被濾掉。此時若不考慮狹縫濾波作用,就會導(dǎo)致自適應(yīng)光學(xué)的過度校正。最后,基于研制的原理樣機(jī)實(shí)驗(yàn)驗(yàn)證了波前像差對高光譜分辨率太陽光柵光譜儀的光譜成像性能的影響。為了研究波前像差對光譜成像性能的影響和自適應(yīng)光學(xué)校正對光譜儀成像性能的影響,本文在太陽光柵光譜儀系統(tǒng)中集成了基于哈特曼波前傳感器HS WFS和液晶空間光調(diào)制器LC-SLM的自適應(yīng)光學(xué)系統(tǒng),對波前像差對光譜成像性能的影響進(jìn)行了定量研究并完成閉環(huán)校正實(shí)驗(yàn)。實(shí)驗(yàn)結(jié)果表明,經(jīng)自適應(yīng)光學(xué)校正后,像差對光譜分辨率的影響可忽略;能量利用率η得到了極大的利用,η≥95%。具有多波段同時成像能力的太陽光柵光譜儀是太陽觀測的重要儀器,而具有高能量利用率和高光譜分辨率的太陽光柵光譜儀對于高精度的太陽大氣活動層析成像觀測和高光譜分辨率的光譜觀測具有重要意義。
[Abstract]:As everyone knows, no information derived from solar magnetic field causes the solar eruptions, such as sunspots, flares and rice. At the same time, and the period of intense solar activity, and influence and modulation of the survival of the human environment. It has important significance for real-time monitoring and forecasting of solar atmosphere and imaging. The grating spectrometer is an important instrument to achieve this goal. It can not only make imaging for the observation of atmospheric activity. At the same time, thermodynamic parameters, and according to the obtained spectral information to determine the outbreak of the solar atmosphere activities such as magnetic field, temperature, pressure and the abundance of elements. Therefore, the grating spectrometer is widely used for observation the atmosphere of the sun. The sun activity grating spectrometer with high spectral resolution of this paper includes the following four parts: the design of high spectral resolution solar grating spectrometer, The development of principle prototype, the wavefront aberration effect on parameters of grating spectrometer and the performance analysis and experimental verification. First, the miniaturized high resolution solar grating spectrometer are studied. Based on the aberration theory, designed a system based on grating spectrometer with high spectral resolution of one meter infrared solar telescope NVST, has the ability of imaging in 656.3nm and at the same time. In order to make the 854.2nm grating spectrometer has good imaging capabilities, the spherical aberration of the grating spectrometer in the coma and astigmatism is compensated. The initial structure of the system, and using the optical design software ZEMAX was optimized. The design results show that the imaging ability of grating spectrometer reaches the diffraction limit this is of great significance for the accurate measurement of thermodynamic parameters of the solar atmosphere and solar atmosphere imaging accurately. Second, high spectral resolution was developed. The sun grating spectrometer principle prototype, from the instrument design, key design elements, a white light spectral resolution spectral measurement and wavelength calibration principle and prototype confirmation, systematically introduces the development method and process of high spectral resolution grating spectrometer. In order to reduce the alignment difficulty of grating spectrometer and better docking with the solar telescope system and we design a calibration source system. In order to eliminate the aberration of the grating spectrograph, we integrated the adaptive optical system in grating spectrometer calibration source system. The experimental results show that the spectral wavelength for the coverage of 0.6 mu m~1.1 mu m; the actual spectral resolution of 5.6pm@632.8nm spectra resolution index has reached the world similar spectral levels. In addition, the spatial resolution of the actual sun grating spectrometer is 55 m, close to the diffraction The spatial resolution of the diffraction limit (50 m). Third, in-depth analysis of the impact of spectral imaging performance of wavefront aberration on high spectral resolution solar grating spectrometer. Unlike general optics, small slit spectrometer, filtering effect has a certain degree of wavefront aberration. Because of this, the mathematical relation between wavefront aberration and spectrum the imaging performance parameters were derived, and the numerical simulation. The results showed: after slit filtering, different types, different sizes of wavefront aberration by spectral resolution and energy rate of different impacts, and compared with the pre filter, wavefront aberration on spectral resolution and energy rate becomes smaller. The slit is small, the stronger the filtering effect. However, the aberration to low frequency such as defocus aberration, the slit is small, the frequency will be filtered out. If not considering the slit filtering effect on Excessive correction will lead to adaptive optics. Finally, the experimental principle developed to verify the spectral imaging performance of wavefront aberration on high spectral resolution grating spectrometer based on the sun. In order to study the effect of wavefront aberration on spectral imaging performance and adaptive optics correction effect on the performance of the imaging spectrometer, in the solar system integrated grating spectrometer the adaptive optical system of Hartmann wavefront sensor WFS and HS liquid crystal spatial light modulator based on LC-SLM, the effect of wavefront aberration on spectral imaging performance was studied quantitatively and the close loop correction experiment. The experimental results show that the adaptive optical correction, the effects of aberration on spectral resolution can be neglected; the energy utilization rate is greatly the ETA = 95%. with multi wavelength grating spectrometer and the sun imaging ability is an important instrument for solar observations Device, and has high energy utilization rate of solar grating spectrometer and high spectral resolution is of great significance for the spectroscopic observations of the solar atmosphere activity tomography measurement with high resolution and high spectral resolution.

【學(xué)位授予單位】：電子科技大學(xué)
【學(xué)位級別】：博士
【學(xué)位授予年份】：2016
【分類號】：TH744.1

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本文編號：1763287