• Current Optics and Photonics
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• 제4권1호
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• pp.50-56
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• 2020

The design of a concentration system for a solar side-pumped slab laser was investigated. The side size of the slab laser medium is 2 mm × 20 mm. Based on the principle of the edge ray, a secondary concentrating system consisting of a rectangular parabolic mirror (RPM) and a rectangular dielectric-filled compound parabolic concentrator (RDCPC) was demonstrated. The focal length of RPM is 1200 mm and the size is 734 mm × 2000 mm. The outlet size of the RDCPC is 2 mm × 20 mm. The concentration effect was analyzed by using Tracepro optical software. The results showed that the concentration efficiency reached 81.3% and the uniformity of the spot was 91.4% after optimization. This design of concentration system is of great reference value for a solar side-pumped slab laser.

• 천문학회보
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• 제39권2호
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• pp.110.1-110.1
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• 2014

The optics of Space telescope is one of the major parts of space mission used for imaging observation of astronomical targets and the Earth. These kinds of space mission have a bulky and complex opto-mechanics with a long optical tube, but there are attempts have been made to observe a target with a small satellite in many ways. In this paper, we describe an optical design of a reflecting telescope for use in a CubeSat mission. For this design, we adopt the off-axis segmented method of astronomical observation techniques based on the Ritchey-Chr$\acute{e}$tien type telescope. The primary mirror shape is a rectangle with dimensions of $8cm{\times}8cm$, and a secondary mirror has dimensions of $2.4cm{\times}4.1cm$. The focal ratio is 3 which can obtain a $0.3{\times}0.2$ degree diagonal angle in a $1280{\times}800$ CMOS color image sensor with a pixel size of $3{\mu}m{\times}3{\mu}m$. This optical design can capture a ${\sim}4km{\times}{\sim}2.3km$ area of the earth's surface at 700 km altitude operation. Based on this conceptual design, we will keep trying to study more for astronomical observation with Attitude control system.

• 대한전기학회:학술대회논문집
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• 대한전기학회 2015년도 제46회 하계학술대회
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• pp.1080-1081
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• 2015

CPV system in the desert areas or areas near the equator, as is suitable for high-temperature region. As compared to silicon solar cells, CPV system have a high proportion of a BOS (balance of system). Solar cells because of its low proportion when designing a module technology is applied in a variety of ways. Applied to the CPV system is classified into two kinds of optical technology. One of those using fresnel lens uses refraction of light energy. The other is a mirror reflection of the structure using sprays. Both of these two ways to condense the sun to collect solar cell is a form of light. And goals by using a small solar cell materials is to produce more energy. This research proposes rational design approach to calculate proper system capacity in consideration of the aforementioned factors in CPV system.

• Journal of the Optical Society of Korea
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• 제17권6호
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• pp.533-537
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• 2013

Space telescope optics is one of the major parts of any space mission used to observe astronomical targets or the Earth. This kind of space mission typically involves bulky and complex opto-mechanics with a long optical tube, but attempts have been made to observe a target with a small satellite. In this paper, we describe the optical design of a reflecting telescope for use in a CubeSat mission. For this design we adopt the off-axis segmented method for astronomical observation techniques based on a Ritchey-Chr$\acute{e}$tien type telescope. The primary mirror shape is a rectangle with dimensions of $8cm{\times}8cm$, and the secondary mirror has dimensions of $2.4cm{\times}4.1cm$. The focal ratio is 3 which can yield a 0.383 degree diagonal angle in a $1280{\times}800$ CMOS color image sensor with a pixel size of $3{\mu}m{\times}3{\mu}m$. This optical design can capture a ${\sim}4km{\times}{\sim}2.3km$ area of the earth's surface at 700 km altitude operation.

• The Journal of the Acoustical Society of Korea
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• 제14권2E호
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• pp.73-86
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• 1995

전향 초음파 영상 캐서터의 트랜스듀스 (FLUIC) 부분은 진동자인 원형 전기음향 소자와 원뿔꼴 반사체인 음향 반사체로 구성된다. 소형의 전기음향 소자는 캐서터의 회전자 축 측면에 탑재된다. 전향 초음파 영상 캐서터의 특징은 기존의 IVUS 트랜스듀서가 제공할 수 없는 캐서터 전단에서 혈관의 단층 2-D 영상과 종래의 측면 영상을 동시에 제공하는 것이다. FLUIC의 트랜스듀서에 사용된 음향 반사체를 설계하기 위해 근사화된 레이 추적 기법을 이용하였다. 음향 반사체로부터 2차 외절 특성을 예측하기 위해 회절전달함수방식에[1] 의한 1차 음원으로 부터의 장 예측모델을 확장하여 일반화 하였다. 확장된 모델은 단순한 평판 반사체에 적용하여 시뮬레이션과 실험에 의해 검증되었으며 FLUIC의 잘 특성을 해석하는데 사용되었다.

• 천문학회지
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• 제51권6호
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• pp.207-214
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• 2018

A coelostat is often used for solar observations, because it corrects the image rotation automatically by guiding sunlight into a fixed telescope with two plane mirrors. For the purposes of education and spectroscopic observation, the solar group at Seoul National University (SNU) plans to develop the SNU coelostat (SNUC) and install it in the SNU Astronomical Observatory (SAO). Requirements of the SNUC are < 1" positioning accuracy with 30 cm beam size on the entrance pupil in the compact dome. To allow for installation in the small dome, we design a compact slope type coelostat with a 45 cm primary plane mirror and a 39 cm secondary plane mirror. The motion of the SNUC is minimized by fixing the position of the slope frame. Numerical simulations of the available observational time of the designed coelostat shows that the sun can be observed ay all times from June to early August and at least three hours in other months. Since the high accuracy driving motors installed in the SNUC can be affected by external environment factors such as humidity and temperature variations, we design a prototype to test the significance of these effects. The prototype consists of a 20 cm primary plane mirror, a 1 m slope rail, a direct drive motor, a ballscrew, a linear motion guide, an AC servo motor, a reduction gear and a linear encoder. We plan to control and test the accuracy of the prototype with varying atmospheric conditions in early 2019. After testing the prototype, the SNUC will be manufactured and installed in SAO by 2020.

• 대한기계학회논문집A
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• 제26권11호
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• pp.2415-2420
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• 2002

In the present study, a new anchor design was proposed to minimize the initial deflection of micro multi-layer cantilever beam with step-up structure, which is a key component of thin film micro-mirror array. It is important to minimize the initial deflection, caused by residual stress, because it reduces the performance of the actuation. Theoretical and experimental studies were conducted to examine the cause of the initial bending deflection. It was found that the bending deflection at the anchor of the cantilever beam was the primary source of initial deflection. Various anchor designs were proposed and the initial deflections for each design were calculated by finite element analysis. The analysis results were compared with experiments. To reduce the initial deflection a secondary support was added to the conventional structure. The optimal shapes were obtained by simulation and experiment. It was found from the analysis that the ratio or horizontal and vertical dimensions of secondary support was the governing factor, which affected the initial deflection.

• 천문학논총
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• 제11권1호
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• pp.163-175
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• 1996

We propose the development and test result of new optical axis alignment system for the interchangeable F/8 secondary mirror of the BOAO 1.8m telescope system. Since the original system was not equipped with a suitable optical alignment facility, the whole alignment process was performed by hand. It was necessary at least three persons working more than 2 nights and the altitude of the telescope could not exceed 10 degrees, in such altitude the alignment quality was not so good by atmospheric effect. The new system adopts position readable motorized system and remote control operation by the computer installed in observation room, which reduces the number of workers to only one and eliminates the altitude restriction. The defocused CCD image pair obtained at higher altitude makes the aberration estimates more accurately and the number of required alignment loops is reduced from 10 to 4. The system has been installed on September 1, and performed alignment three times. The test results show that the system is stable and accurate, gives better optical performance of the telescope under F/8 focus. We hope to emphasize the fact that the new system will increase observation time of the telescope by about 20 nights per year assuming one alignment in every month.

• 에너지공학
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• 제23권4호
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• pp.56-60
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• 2014

태양추적 장치에 장착된 집광기를 이용하여 획득한 고밀도의 태양광에너지는 적외선 범위 및 가시광선 범위의 두 파장 영역으로 분리할 수 있다. 적외선 범위의 파장은 열음향 시스템으로 활용할 수 있으며, 가시광선 범위의 파장은 조명시스템을 통하여 실내 태양광 조명에 활용할 수 있다. 즉, 집광된 태양광은 2차 반사경을 통해 광분리 장치로 입사되며, 입사된 태양광은 Hot mirror를 통하여 가시광선 영역과 적외선 영역으로 분리된다. 본 연구에서는 자연 태양광 및 실내의 인공광원을 대상으로 분리 실험을 하였다. 실내 광원 발생장치 실험에서 분리된 인공광원이 가시광선 영역의 파장은 400m부터 720m 범위이며, 적외선 영역의 파장은 620m부터 940m 범위이다. 또한, 태양추적 장치의 집광된 태양광을 통한 실험에서 가시광선 영역의 파장은 460m부터 680m 범위를 보이며, 적외선 영역의 파장은 620m부터 940m 범위인 것을 확인하였다.

• 한국광학회지
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• 제22권6호
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• pp.262-268
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• 2011

한국천문연구원이 개발한 다목적적외선영상시스템(Multi-purpose IR Imaging System, MIRIS)은 과학기술위성 3호(STSAT-3)의 주탑재체이다. 지구관측카메라(Earth Observation Camera, EOC)는 MIRIS를 구성하는 두 개의 적외선 카메라 중에 하나로, 지구의 $3{\sim}5{\mu}m$ 파장대의 적외선을 관측하기 위한 카메라이다. EOC의 광학계는 카세그레인 방식으로써 구경이 100 mm이고, 주경과 부경은 모두 비구면 반사경이다. EOC 주경의 플렉서는 링 타입으로써 발사환경에서 주경이 겪을 수 있는 충격과 진동을 견디도록 예압을 가하며 주경을 지지한다. 이는 마치 리테이너로 렌즈를 지지하는 것과 같은 메커니즘으로 주경을 지지하기 위한 시도이다. 광기계 해석을 통해 EOC 주경이 효과적으로 지지되고 있음을 확인했다.