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Distinct synergetic effects in the ozone enhanced photocatalytic degradation of phenol and oxalic acid with Fe3+/TiO2 catalyst 会议论文
Collaborat Innovat Ctr Chem Sci & Engn, Tianjin, PEOPLES R CHINA, JUL 12-15, 2015
作者:  Xie, Yongbing;  Chen, Yingying;  Yang, Jin;  Liu, Chenming;  Zhao, He
收藏  |  浏览/下载：41/0  |  提交时间：2019/06/21
Engineered Bamboo's Further Application: An Empirical Study in China 会议论文
作者:  Xing, W.Q.;  Hao, J.L.;  Galobardes, I.;  Wei, S.B.;  Chen, Z.T.
收藏  |  浏览/下载：2/0  |  提交时间：2019/11/26
Study of ultraviolet assisted cure mechanism of the phosphor/silicone composites used in White LEDs 会议论文
Proceedings - 2018 19th International Conference on Electronic Packaging Technology, ICEPT 2018
作者:  Wang, Z.;  Fan, J.;  Liu, J.;  Hu, A.;  Qian, C.
收藏  |  浏览/下载：11/0  |  提交时间：2019/12/30
Feasibility analysis on integration of luminous environment measuring and design based on exposure curve calibration 会议论文
5th International Conference on Machine Vision (ICMV) - Computer Vision, Image Analysis and Processing, Wuhan, PEOPLES R CHINA, OCT 20-21, 2012
作者:  Zou, Yuan*;  Shen, Tianxing
收藏  |  浏览/下载：9/0  |  提交时间：2019/12/04
Design of the real-time autofocusing system for collimator with long focus length and large aperture (EI CONFERENCE) 会议论文
2011 International Academic Conference on Numbers, Intelligence, Manufacturing Technology and Machinery Automation, MAMT 2011, December 24, 2011 - December 25, 2011, Wuhan, China
Li X.; Zhang X.
收藏  |  浏览/下载：34/0  |  提交时间：2013/03/25
Large aperture collimator which has been widely used for calibrating and testing various optical devices plays an essential role in correlative laboratories. As being the basic testing and calibration equipment  the large aperture collimator's accuracy should be much higher than the device under testing in order to ensure the accuracy of the measurement. However  the process of adjusting the collimator is extremely complicated due to the collimator's large aperture and long focal length. So it is difficult to ensure the measurement's quality and easy to cause the system being vulnerable to the surrounding environment. One of the most common problems is defocus. In order to solve the problem above  this issue presents a new type of autocollimator autofocusing system which uses pentaprism instead of using large-aperture plane mirror  semiconductor lasers as light source and CCD sensor as receiver. The system is smaller  lighter  and more convenient when using. The computer simulation shows that the autofocusing system's resolution could reach the accuracy of 40m. If we use the relevant algorithms to execute the sub-pixel scanning  the resolution could reach the accuracy of 10m. It shows that the system could satisfy the required testing precision of testing large aperture optical device.  
Gimbal displacement error analysis on an electro-optical seeker (EI CONFERENCE) 会议论文
Optical Design and Testing IV, October 18, 2010 - October 20, 2010, Beijing, China
Jiang Z.; Zhang X.; Ai X.; Wei Q.; Jia H.
收藏  |  浏览/下载：23/0  |  提交时间：2013/03/25
It is essential to analyze the gimbal displacement errors for a seeker due to the importance for cueing of targets and tracking for the final approach. Otherwise  for a seeker electro-driven with a concentric glass dome  the large errors will decrease the picking  pointing  and tracking precision rooted from the displacement errors existing between the rotation center of the optical system and the gimbal. And the gimbaled camera system displacement errors are never eliminated but reduced due to the geometric errors consists of geometric tolerances of gimbal structure  manufacture  installation and vibration coming from working environment. In this paper  the gimbal displacement errors in an electro-optically stabilized platform resulting from geometric errors and environment errors were analyzed and shown in detail. The mathematical modal of the gimbal displacement errors created based on multi-body dynamics demonstrated the connection between the gimbal displacement errors and the stabilized platform. Taking a visible light image seeker as a case  the diameter is 120mm  and the geometric tolerances came from the values of primary design and the vibration data came from the environmental vibration test on the pitch-yaw seeker  and at the same time  the errors resulting from installation were considered too. Based on calculating  the maximum gimbal displacement error will reach to 0.2mm for pitching angle smaller than 40 and yawing angle smaller than 60. However  the critical parts have been found out according to the probability theory and the reliability analysis successfully used in the paper  and finally  the maximum gimbal displacement error reduced to 0.1mm  which is acceptable corresponding to the picking  pointing and tracking precision for an optical imaging seeker. 2010 Copyright SPIE - The International Society for Optical Engineering.  
Design of high precision star image locating method used in star sensor technology (EI CONFERENCE) 会议论文
2010 International Conference on Computer, Mechatronics, Control and Electronic Engineering, CMCE 2010, August 24, 2010 - August 26, 2010, Changchun, China
Zhang S.; Sun H.; Wang Y.; Jia X.; Chen H.
收藏  |  浏览/下载：50/0  |  提交时间：2013/03/25
Nowadays star sensor technology used in aircraft attitude measurement has become more and more popular for its high precision  light weight  without attitude accumulation errors and other advantages. In order to enhance the accuracy of star sensor  it is critical to make efforts to promote the precision of star image locating. High precision star image locating method mentioned in this article includes two aspects. One is sub-pixel dividing algorithm used to acquire the coordinate of stars. The other one is imaging calibration method used to weaken the effect caused by imaging distortion. This method is finally realized in some type of star sensor system. Then an experiment is designed to verify the precision of the method. The result of the experiment shows that the precision of the method is 2" in the experimental environment. 2010 IEEE.  
The calibration of faint simulation star magnitude based on single photon count technique (EI CONFERENCE) 会议论文
International Symposium on Photoelectronic Detection and Imaging 2009: Advances in Imaging Detectors and Applications, June 17, 2009 - June 19, 2009, Beijing, China
Gan X.-J.; Guo J.; Xu S.-Y.
收藏  |  浏览/下载：20/0  |  提交时间：2013/03/25
A calibration method of faint star magnitude of the star scene simulation device is proposed in this paper. In the research of simulation star magnitude  luminometers and CCD devices are the general calibration devices which are used to measure the illumination intensity and calibrate its magnitude. But if the simulation magnitude is only sixth magnitude  its illumination intensity is only 1.010-8 Lux. This illumination intensity level is the lowest illumination intensity that the commercial luminometer can detect. Hence the simulation star magnitude lower than six magnitude cannot be calibrated by luminoters. Likewise CCD devices also need an additive cooler in this case. When the single photon characteristic is presented due to the low luminosity of simulating light sources  the simulation star magnitude can be calibrated by detecting its photon flux of radiation with the method of single photon count. In this paper the detection principle of single photon based on a compact designed PMT detecting of the radiation level of simulation star magnitude is advanced. Especially a spectrum match method is proved theoretically to be an effective means for selecting PMT photosensitive type. In the case of the detection object of the simulation star in visible wavelength  a analysis indicates that the material of tri-alkali cathode materials its best choice after being compared the Signal-to-Noise of photon detector of several PMT photosensitive materials based on the different spectrum match ratio of different object light sources and different cathode materials. An experiment is employed to show the relationship of control voltage of PMT and its dark counter  the relationship of the environment temperature of PMT and its dark counter  which proves its only decades of CPS at room temperature. The so low dark counter avoids a bulky cooler and is convenient for installing it on the star scene simulation equipment. Finally in the experiment of calibrating the simulation star magnitudes the ability of its calibration is confirmed to reaches up to 12m  meanwhile its calibration error is within 0.2m. 2009 SPIE.  
Research on the support structure of the primary mirror of large-aperture telescope (EI CONFERENCE) 会议论文
3rd International Symposium on Advanced Optical Manufacturing and Testing Technologies, AOMATT 2007: Large Mirrors and Telescopes, July 8, 2007 - July 12, 2007, Chengdu, China
Yang W.; Jingxu Z.
收藏  |  浏览/下载：21/0  |  提交时间：2013/03/25
Large-aperture telescope can be used in surveying battlefield  researching landform  searching object  real-time monitoring  imaging  detecting and identifying spatial targets and so on. A large-aperture telescope for achieving high resolution power is designed to monitor spatial target and image in real time. Real-time monitoring plays an important role in military conflicts. The orbit parameter of object  quantity  geometrical shape parameter and so on can be obtained by detect spatial target. With the development of optical technology  people require larger aperture in optics-electronic (OE) system. By increasing optical aperture  the ability of collecting light and resolution power in the system can be enhanced. But the support structure of the primary mirror of large-aperture telescope will be a very difficult problem. With the increase of primary mirror aperture  the weight of the primary mirror will become larger than before. The root mean square (rms) of the primary mirror is affected by many factors  such as deadweight  deformation of heat  environment and so on. Due to the primary mirror of telescope is an important component of telescope system. By reducing the weight of primary mirror  precision of the system is ensured. During the designing phase  one can consider the supporting project of the primary mirror synthetically and analyze it roundly according to technical requirement of optical system and the effect factors. The final structural design can be reasonable. In an astronomical telescope  the surface of reflector is an important part for collecting dark radiation of celestial bodies. Its surface shape will have an effect on collecting efficiency of telescope radiant energy directly. So the rms must be very high. Optical system of large aperture  small wavelength and small focus can receive maximal light intensity. For ground-based optical astronomical telescope  the design proposed in the paper can satisfy the requirement of the possible minimum atmosphere seeing at astronomical observatory site and exert the use efficiency of the telescope adequately. So the accuracy of the traditional surface of reflector can assure that 90% of all the light energy can be focused on within the angle diameter range of the minimum atmosphere seeing  then 100% of light energy should be focused on the angle diameter range of minimum atmosphere seeing. Because the rms of mirror is very high  precise surface machining and accurate the support of mirror are very important tasks during designing and manufacturing the telescope. In the paper  various support techniques of a large-aperture telescope primary mirror are discussed and a 3.5 meter telescope system at the Starfire Optical Range (SOR) overviewed simply  which was operated by the Directed Energy Directorate of the Air Force Research Laboratory  Kirtland AFB  NM  USA from the ground-based O-E system for the observations of spatial target. We also analyze Theoretical elastic deformation of the Steward Observatory 2.3 meter mirror is analyzed.  

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