蜂窝镜温度与镜面视宁度控制方法研究
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摘要
温度是影响大口径天文望远镜高分辨力成像质量的关键因素之一。当环境温度快速变化时，在温度差的作用下望远镜主镜与环境空气之间发生热量交换。导致主镜表面空气的对流扰动，形成主镜视宁度现象对成像质量造成严重影响。减小主镜视宁度对望远镜高分辨力成像质量的影响是本文研究的主要目的。
根据主镜视宁度产生的物理机理，目前对主镜视宁度控制的常用方法主要有两种：一种方法是控制主镜自身的温度，使主镜反射表面与环境空气温度差维持在一定范围内；另外一种方法是在平行于主镜前表面的方向吹风，用一层薄薄的均匀流动的“气刀”将主镜视宁度扰动抚平。
本文通过温度场的计算，结合国外主镜视宁度计算经验公式，分别对实心镜面和蜂窝镜面主镜视宁度现象的定量计算和改善效果进行了研究。运用温度场理论对实心镜面主镜视宁度及“气刀”改善效果进行了详细的研究。提出了一种灵活多变、可操作性强的蜂窝镜面温度控制方案。提出了用于大口径蜂窝镜面温度控制研究的单蜂窝单元假设。以四米蜂窝镜面为例，运用计算流体动力学方法和有限元方法对蜂窝镜面温度场和热变形进行了计算。从主镜视宁度和热变形两个方面对四米蜂窝镜面温度控制效果进行了分析。对四米蜂窝镜面温度控制具体工程问题进行了研究。建立“气刀”流场模型，对气刀流场特性及其引入的光学像差进行了计算。
通过本论文的研究，摸索出一整套用于主镜视宁度和温度控制研究的技术路线。为我国未来研制更大口径高分辨力成像望远镜在主镜温度控制方面奠定了坚实的基础。
Temperature is one of the key factors which affect the high resolution image quality oflarge aperture astronomical telescope. When ambient temperature varies quickly, heattransfer appears between primary mirror blank and the ambient air because oftemperature difference. Primary mirror seeing result from the air turbulence of heatconvection, may derange the atmosphere along the optical path, and lead to opticalaberrations and awful image quality. Minimum primary mirror seeing phenomenon’seffect on the high resolution image quality of large aperture astronomical telescope isthe main purpose of the dissertation.According to physical principle of primary mirror seeing, there are two commonmethods to control primary mirror seeing. One method is control the temperature ofprimary mirror, making the temperature difference between the reflecting surface ofprimary mirror and ambient air in a small range; another is using “air knife” alongreflecting surface of primary mirror to minimize the turbulence of primary mirrorseeing.
In this paper, primary mirror seeing and its improvement effect of classical mirror andhoneycomb mirror are studied by thermal field calculation and empirical equationabout primary mirror seeing. Primary mirror seeing quantitative calculation and “airknife” effect of classical mirror are analyzed through temperature field analyticalsolution in detail. A flexible and easy operational thermal control method is presented.A single honeycomb cell model hypothesis is introduced for large aperturehoneycomb mirror thermal control system research. Taking the4m honeycomb mirrorfor example, computational fluid dynamics and finite element method are used tocalculate the honeycomb mirror temperature field and thermal deformation.4mhoneycomb mirror thermal control effect is analyzed in primary mirror seeing andthermal deformation two aspects. Some specific engineering problems in4mhoneycomb mirror thermal control system are discussed.“Air knife” flow model isintroduced to calculate the “air knife” flow field characteristics and the opticalaberrations result from air flow.
Through this research, a whole set of technical method which is used to controlprimary mirror seeing and temperature has been worked out. These methods used inthis paper lay a strong foundation for the future development of larger aperture highresolution image telescope in the primary mirror temperature control aspect.
根据主镜视宁度产生的物理机理，目前对主镜视宁度控制的常用方法主要有两种：一种方法是控制主镜自身的温度，使主镜反射表面与环境空气温度差维持在一定范围内；另外一种方法是在平行于主镜前表面的方向吹风，用一层薄薄的均匀流动的“气刀”将主镜视宁度扰动抚平。
本文通过温度场的计算，结合国外主镜视宁度计算经验公式，分别对实心镜面和蜂窝镜面主镜视宁度现象的定量计算和改善效果进行了研究。运用温度场理论对实心镜面主镜视宁度及“气刀”改善效果进行了详细的研究。提出了一种灵活多变、可操作性强的蜂窝镜面温度控制方案。提出了用于大口径蜂窝镜面温度控制研究的单蜂窝单元假设。以四米蜂窝镜面为例，运用计算流体动力学方法和有限元方法对蜂窝镜面温度场和热变形进行了计算。从主镜视宁度和热变形两个方面对四米蜂窝镜面温度控制效果进行了分析。对四米蜂窝镜面温度控制具体工程问题进行了研究。建立“气刀”流场模型，对气刀流场特性及其引入的光学像差进行了计算。
通过本论文的研究，摸索出一整套用于主镜视宁度和温度控制研究的技术路线。为我国未来研制更大口径高分辨力成像望远镜在主镜温度控制方面奠定了坚实的基础。
Temperature is one of the key factors which affect the high resolution image quality oflarge aperture astronomical telescope. When ambient temperature varies quickly, heattransfer appears between primary mirror blank and the ambient air because oftemperature difference. Primary mirror seeing result from the air turbulence of heatconvection, may derange the atmosphere along the optical path, and lead to opticalaberrations and awful image quality. Minimum primary mirror seeing phenomenon’seffect on the high resolution image quality of large aperture astronomical telescope isthe main purpose of the dissertation.According to physical principle of primary mirror seeing, there are two commonmethods to control primary mirror seeing. One method is control the temperature ofprimary mirror, making the temperature difference between the reflecting surface ofprimary mirror and ambient air in a small range; another is using “air knife” alongreflecting surface of primary mirror to minimize the turbulence of primary mirrorseeing.
In this paper, primary mirror seeing and its improvement effect of classical mirror andhoneycomb mirror are studied by thermal field calculation and empirical equationabout primary mirror seeing. Primary mirror seeing quantitative calculation and “airknife” effect of classical mirror are analyzed through temperature field analyticalsolution in detail. A flexible and easy operational thermal control method is presented.A single honeycomb cell model hypothesis is introduced for large aperturehoneycomb mirror thermal control system research. Taking the4m honeycomb mirrorfor example, computational fluid dynamics and finite element method are used tocalculate the honeycomb mirror temperature field and thermal deformation.4mhoneycomb mirror thermal control effect is analyzed in primary mirror seeing andthermal deformation two aspects. Some specific engineering problems in4mhoneycomb mirror thermal control system are discussed.“Air knife” flow model isintroduced to calculate the “air knife” flow field characteristics and the opticalaberrations result from air flow.
Through this research, a whole set of technical method which is used to controlprimary mirror seeing and temperature has been worked out. These methods used inthis paper lay a strong foundation for the future development of larger aperture highresolution image telescope in the primary mirror temperature control aspect.
引文
[1]詹子庆.中国古代史，北京：高等教育出版社，2003年，第二版，上册：125.
[2]卞毓麟.光学天文望远镜的足迹，上海：上海科技教育出版社，2008年第12期：844～852
[3]程景全.天文望远镜原理和设计.北京：中国科学技术出版社，2003：9，60～71.
[4]崔向群.LAMOST项目及进展.天文学进展，2001年，第19卷，第2期：123～128.
[5]朱毅麟.追踪宇宙第一道光.国际太空,2004年，11月号：4～7.
[6]姜文汉，张雨东，饶长辉，凌宁等.中国科学院光电技术研究所的自适应光学研究进展.光学学报.2011年，第31卷，第9期：0900106-1～0900106-9.
[7] Masanori lye and Keiichi Kodaira. Primary mirror support system for the SUBARUtelescope[C]. SPIE Vol.2199,762～763.
[8] Keizo Miyawaki, Noboru Itoh, Ryuichi Sugiyama, etc. Mechanical structure forthe SUBARU telescope [J]. SPIE, Vol.2199,754～761.
[9] Pierre Y. Bely.The Design and Construction of Large Optical Telescopes[M].NewYork. Springer Press，2002.
[10] Woolf N.J. Seeing and the design and location of a15meter telescope.SPIEVol.332.Advanced Technology Optical Telescopes.1982:193～197.
[11] Woolf N.J. High resolution imaging form the ground. Ann. Rev. Astron. Astrophys.1982:367～398.
[12] Racine R.Astronomical seeing at Mauna Kea and in particular at CFHT，Proc.IAUColloquium No.79，Garching April9-12，1984.
[13] Zago, L. The effects of the local atmospheric environment on astronomicalobservations.PhD thesis. Swiss Federal Institute of Technology,(EPFL),Switzerland,1995.
[14] Zago, Lorenzo.“An engineering handbook for local and dome seeing”.Proc.SPIE, vol.2871, p.726,1997.
[15] Tirupathi R.Chandrupatla, Ashok D. Belegundu. Introduction to Finite Elementsin Engineering[M].Beijing: China Machine Press.2005:84～85.
[16] Walter A.Siegmund and Charles Comfort.Design of the Apache Point Observatory3.5m telescope Ⅰ.Thermal control of the telescope enclosure.1986.SPIE.Vol.628:369～376
[17] G. G. Williamsa, J. D. Gibsona, S. Callahanb,D. Blancoa, J. T. Williamsa,b,and P. Spencera. Performance and control of the MMT thermal system.2004.SPIEVol.5489:938～943.
[18] Larry W Goble. Temperature control of the3.5-Meter WIYN telescope primarymirror.SPIE Vol.1532:161～169.
[19] J. D. Gibson, G. G. Williams, S. Callahan et al.. Advances in thermal controland performance of the MMT M1mirror. SPIE Vol.7733:77333Y1～12
[20]童骏耕.工程热力学.北京：高等教育出版社，第四版，2007年：142～145.
[21]杨世铭，陶文铨.传热学.北京：高等教育出版社，第四版，2006：3～12.
[22]贾力,方肇洪.高等传热学.北京：高等教育出版社，第二版，2008：74～78.
[23]谈庆明.量纲分析.合肥：中国科学技术大学出版社，2005年：12～15.
[24]张继恒，刘彬生.近代物理课外实验.1989
[25] Cengel Y A.Heat transfer, A Practical approach. Boston: WCB McGraw-Hill,1998:228.
[26] Holman J P. Heat transfer.9th ed. Boston: WCB McGraw-Hill,2002:285～287.
[27] Incropera F P, DeWitt D P. Fundamentals of heat and mass transfer.5th ed.2002:430,482,492,546,551.
[28] Incropera F P. DeWitt D P. Fundamentals of heat and mass transfer[M].5th ed.John Wiley&Sons,2002:430,546,551.
[29] F.P.Incropera. D.P.DeWitt. Fundamentals of Heat and Mass Transfer[M]. SixthEdition. John Wiley&Son,2007:363:370.
[30]陶文铨.数值传热学.北京：西安交通大学出版社，2001：1～5.
[31]林建忠，阮晓东，陈邦国等.流体力学.北京：清华大学出版社，2005年：82～99.
[32]王福军.计算流体动力学分析.北京：清华大学出版，2004年：6～12.
[33]郝允祥,陈培生,周克平.红外天文学导论.北京：北京大学出版社.1993.66
[34] Tirupathi R.Chandrupatla, Ashok D. Belegundu. Introduction to Finite Elementsin Engineering[M].Beijing: China Machine Press.2005:84～85.
[35]王勖成，邵敏.有限单元法基本原理和数值方法.北京：清华大学出版社.1997：38～122.
[36] J.M.Rüeger. Rerfactive Indices of Light，Inrfared and Radio Waves in theAtmosphere. Report of the Ad-Hoc Working Party of the IAG Special Commission SC3on Fundamental Constnats[C],1993-1999,22nd General Assembly of IUGG, Birminghma,UK,18-30July l999,25Pages.
[37] J.M.Rüeger. Rerfactive Indices of Light，Inrfared and Radio Waves in theAtmosphere. Report of the Ad-Hoc Working Party of the IAG Special Commission SC3on Fundamental Parmaeters (SCFC)[C],1999-2003，23rd General Assembly of IUGGSapporo, Japan,30June-ll july2003,6pages.
[38]金群峰.大气折射率影响因素的研究[D].杭州：浙江大学信息学院,2006：8～18.
[39]张逸新,迟泽英.光波在大气中的传输与成像[M].国防工业出版社.北京：1997年7月1版：8～9.
[40]魏在福，查鸿逵，王润文.激光加热温度场物理分析[J].光学学报，1994，14（4）：355～359
[41]赵强，范正修.光学薄膜界面吸收对温度场的影响[J].光学学报，1996,16(6):777～782
[42]赵强，范正修，王之江.激光对光学薄膜加热过程的数值分析[J].光学学报，1999,19(8):1019～1023
[43]陆培华，王润文.高功率激光器窗口三维温度场分析及其热透镜研究[J].光学学报，2001，21(8):965～969
[44] Frank-M. G ttsche, Folke S. Olesen. Modelling of diurnal cycles of brightnesstemperature extracted from METEOSAT data[J]. Remote Sensing ofEnvironment.2001.76(2001):337-348
[45]张俊、鲜浩、贺元兴、饶长辉.望远镜主镜温度场理论计算及主镜视宁度分析[J].光学学报，2012，32（10）：1022001-1～7.
[46]杨力，方敬忠等.先进光学制造技术[M].北京：科学出版社，2001：第196～198页.
[47]王艳茹光学元件吸收损耗和热变形检测技术研究博士学位论文北京：中国科学院研究生院.2011：60-80.
[48] Anderson D A，Tannehill J C，Pletcher R H.Computational fluid mechanics andheat transfer. Washington DC：Hemisphere，1984.199～201.
[49] Rodi W. Recent developments in turbulent modeling. In：’93workshop onmathematical modeling of turbulent flows,1993. Tokyo,1.1～1.48.
[50]谢龙汉，赵新宇，张炯明.ANSYS CFX流体分析及仿真.北京：电子工业出版社.2012年：12～18.
[51]中国市政工程东北设计研究院，给排水设计手册（第一册）常用资料[M].中国建筑工业出版社.2000
[52]暖通空调常用数据手册[M].中国建筑工业出版社.2002：717
[2]卞毓麟.光学天文望远镜的足迹，上海：上海科技教育出版社，2008年第12期：844～852
[3]程景全.天文望远镜原理和设计.北京：中国科学技术出版社，2003：9，60～71.
[4]崔向群.LAMOST项目及进展.天文学进展，2001年，第19卷，第2期：123～128.
[5]朱毅麟.追踪宇宙第一道光.国际太空,2004年，11月号：4～7.
[6]姜文汉，张雨东，饶长辉，凌宁等.中国科学院光电技术研究所的自适应光学研究进展.光学学报.2011年，第31卷，第9期：0900106-1～0900106-9.
[7] Masanori lye and Keiichi Kodaira. Primary mirror support system for the SUBARUtelescope[C]. SPIE Vol.2199,762～763.
[8] Keizo Miyawaki, Noboru Itoh, Ryuichi Sugiyama, etc. Mechanical structure forthe SUBARU telescope [J]. SPIE, Vol.2199,754～761.
[9] Pierre Y. Bely.The Design and Construction of Large Optical Telescopes[M].NewYork. Springer Press，2002.
[10] Woolf N.J. Seeing and the design and location of a15meter telescope.SPIEVol.332.Advanced Technology Optical Telescopes.1982:193～197.
[11] Woolf N.J. High resolution imaging form the ground. Ann. Rev. Astron. Astrophys.1982:367～398.
[12] Racine R.Astronomical seeing at Mauna Kea and in particular at CFHT，Proc.IAUColloquium No.79，Garching April9-12，1984.
[13] Zago, L. The effects of the local atmospheric environment on astronomicalobservations.PhD thesis. Swiss Federal Institute of Technology,(EPFL),Switzerland,1995.
[14] Zago, Lorenzo.“An engineering handbook for local and dome seeing”.Proc.SPIE, vol.2871, p.726,1997.
[15] Tirupathi R.Chandrupatla, Ashok D. Belegundu. Introduction to Finite Elementsin Engineering[M].Beijing: China Machine Press.2005:84～85.
[16] Walter A.Siegmund and Charles Comfort.Design of the Apache Point Observatory3.5m telescope Ⅰ.Thermal control of the telescope enclosure.1986.SPIE.Vol.628:369～376
[17] G. G. Williamsa, J. D. Gibsona, S. Callahanb,D. Blancoa, J. T. Williamsa,b,and P. Spencera. Performance and control of the MMT thermal system.2004.SPIEVol.5489:938～943.
[18] Larry W Goble. Temperature control of the3.5-Meter WIYN telescope primarymirror.SPIE Vol.1532:161～169.
[19] J. D. Gibson, G. G. Williams, S. Callahan et al.. Advances in thermal controland performance of the MMT M1mirror. SPIE Vol.7733:77333Y1～12
[20]童骏耕.工程热力学.北京：高等教育出版社，第四版，2007年：142～145.
[21]杨世铭，陶文铨.传热学.北京：高等教育出版社，第四版，2006：3～12.
[22]贾力,方肇洪.高等传热学.北京：高等教育出版社，第二版，2008：74～78.
[23]谈庆明.量纲分析.合肥：中国科学技术大学出版社，2005年：12～15.
[24]张继恒，刘彬生.近代物理课外实验.1989
[25] Cengel Y A.Heat transfer, A Practical approach. Boston: WCB McGraw-Hill,1998:228.
[26] Holman J P. Heat transfer.9th ed. Boston: WCB McGraw-Hill,2002:285～287.
[27] Incropera F P, DeWitt D P. Fundamentals of heat and mass transfer.5th ed.2002:430,482,492,546,551.
[28] Incropera F P. DeWitt D P. Fundamentals of heat and mass transfer[M].5th ed.John Wiley&Sons,2002:430,546,551.
[29] F.P.Incropera. D.P.DeWitt. Fundamentals of Heat and Mass Transfer[M]. SixthEdition. John Wiley&Son,2007:363:370.
[30]陶文铨.数值传热学.北京：西安交通大学出版社，2001：1～5.
[31]林建忠，阮晓东，陈邦国等.流体力学.北京：清华大学出版社，2005年：82～99.
[32]王福军.计算流体动力学分析.北京：清华大学出版，2004年：6～12.
[33]郝允祥,陈培生,周克平.红外天文学导论.北京：北京大学出版社.1993.66
[34] Tirupathi R.Chandrupatla, Ashok D. Belegundu. Introduction to Finite Elementsin Engineering[M].Beijing: China Machine Press.2005:84～85.
[35]王勖成，邵敏.有限单元法基本原理和数值方法.北京：清华大学出版社.1997：38～122.
[36] J.M.Rüeger. Rerfactive Indices of Light，Inrfared and Radio Waves in theAtmosphere. Report of the Ad-Hoc Working Party of the IAG Special Commission SC3on Fundamental Constnats[C],1993-1999,22nd General Assembly of IUGG, Birminghma,UK,18-30July l999,25Pages.
[37] J.M.Rüeger. Rerfactive Indices of Light，Inrfared and Radio Waves in theAtmosphere. Report of the Ad-Hoc Working Party of the IAG Special Commission SC3on Fundamental Parmaeters (SCFC)[C],1999-2003，23rd General Assembly of IUGGSapporo, Japan,30June-ll july2003,6pages.
[38]金群峰.大气折射率影响因素的研究[D].杭州：浙江大学信息学院,2006：8～18.
[39]张逸新,迟泽英.光波在大气中的传输与成像[M].国防工业出版社.北京：1997年7月1版：8～9.
[40]魏在福，查鸿逵，王润文.激光加热温度场物理分析[J].光学学报，1994，14（4）：355～359
[41]赵强，范正修.光学薄膜界面吸收对温度场的影响[J].光学学报，1996,16(6):777～782
[42]赵强，范正修，王之江.激光对光学薄膜加热过程的数值分析[J].光学学报，1999,19(8):1019～1023
[43]陆培华，王润文.高功率激光器窗口三维温度场分析及其热透镜研究[J].光学学报，2001，21(8):965～969
[44] Frank-M. G ttsche, Folke S. Olesen. Modelling of diurnal cycles of brightnesstemperature extracted from METEOSAT data[J]. Remote Sensing ofEnvironment.2001.76(2001):337-348
[45]张俊、鲜浩、贺元兴、饶长辉.望远镜主镜温度场理论计算及主镜视宁度分析[J].光学学报，2012，32（10）：1022001-1～7.
[46]杨力，方敬忠等.先进光学制造技术[M].北京：科学出版社，2001：第196～198页.
[47]王艳茹光学元件吸收损耗和热变形检测技术研究博士学位论文北京：中国科学院研究生院.2011：60-80.
[48] Anderson D A，Tannehill J C，Pletcher R H.Computational fluid mechanics andheat transfer. Washington DC：Hemisphere，1984.199～201.
[49] Rodi W. Recent developments in turbulent modeling. In：’93workshop onmathematical modeling of turbulent flows,1993. Tokyo,1.1～1.48.
[50]谢龙汉，赵新宇，张炯明.ANSYS CFX流体分析及仿真.北京：电子工业出版社.2012年：12～18.
[51]中国市政工程东北设计研究院，给排水设计手册（第一册）常用资料[M].中国建筑工业出版社.2000
[52]暖通空调常用数据手册[M].中国建筑工业出版社.2002：717
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