• 우주기술과 응용
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• 제4권3호
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• pp.185-198
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• 2024

Korea Astronomy and Space science Institute (KASI) partnered with the Australian National University (ANU) to develop the adaptive optics (AO) system at the Geochang observatory with a 100 cm optical telescope for multiple applications, including space geodesy, space situational awareness and Korean space missions. The AO system is designed to get high resolution images of space objects with lower magnitude than 10 by using themselves as a natural guide star, and achieve a Strehl ratio larger than 20% in the environment of good seeing with a fried parameter of 12-15 cm. It will provide the imaging of space objects up to 1,000 km as well as its information including size, shape and orientation to improve its orbit prediction precision for collision avoidance between active satellites and space debris. In this paper, we address not only the design of AO system, but also analyze the images of stellar objects. It is also demonstrated that the AO System is achievable to a near diffraction limited full width at half maximum (FWHM) by analyzing stellar images.

• 대한두개안면성형외과학회지
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• 제10권2호
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• pp.81-85
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• 2009

Purpose: The inferior orbital wall is the most vulnerable to injury and inadequate reconstruction of inferior orbital fracture result in postoperative complications include enophthalmos, ocular dystopia and diplopia. Although the anatomical reconstruction of the inferior orbital wall is necessary to prevent these complications, the complexity of inferior orbital wall makes it difficult. We fabricated and remodeled the titanium micro-mesh plate for the anatomical reconstruction of inferior orbital wall. Methods: Twenty-nine patients with inferior orbital wall blow-out fracture were operated and twelve of them presented large extensive fracture. We intraoperatively fabricated and remodeled the Titanium-micro mesh to angulated lazy S shape similar to contralateral uninjured orbit. The preoperative and postoperative facial CT scan verified the 3-dimensional and anatomical reconstruction of the fractures. The mean follow-up was 19.7 months and postoperative complications was evaluated. Results: All cases showed the exact anatomical reconstruction, but there were minor complications in two cases. one patient had postoperative diplopia until 3months after surgery and the other patient had persistent enophthalmos (2 mm), but no further surgical correction was required. Conclusion: The comprehensive understanding of orbital convexity is the most important factor for anatomical reconstruction of inferior orbital fracture. We could prevent postoperative complications after inferior orbital wall reconstruction by intraoperative fabrication and anatomical remodeling of Titanium micro-mesh.

• 대한두개안면성형외과학회지
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• 제21권4호
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• pp.219-224
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• 2020

Background: Repair of the orbital floor following trauma or tumor removal remains a challenge because of its complex three-dimensional shape. The purpose of the present study is to understand normal orbital floor anatomy by investigating its differences across four groups (Caucasian American and East Asian, males and females) via facial bone computed tomography (CT). Methods: A total of 48 orbits in 24 patients between 20 and 60 years of age were evaluated. Although most patients underwent CT scanning following trauma, the orbital walls were intact in all patients. Linear and angular measurements of the orbital floor were obtained from CT images. Results: Orbital floor width, length, angle between the orbital floor and medial wall, and distance from the inferior orbital rim to the lowest point of the orbital floor did not show a statistically significant difference between groups. Angles made by the infraorbital rim, the lowest point of the floor, and the anterior border of the infraorbital fissure were statistically significantly wider in East Asian females than in male groups. The floor depth in East Asian females was significantly smaller compared to all the other groups. Conclusion: East Asian female population had smaller curvature and depth of an orbital floor than the other groups, which means racial and sex-related differences should be considered in the orbital floor reconstruction.

• 천문학회보
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• 제42권2호
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• pp.48.3-49
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• 2017

Interplanetary space of the solar system contains a large number of dust particles, referred to as Interplanetary Dust Particles (IDPs) cloud complex. They are observable through meteors and zodiacal lights. The relative contribution of possible sources to the IDPs cloud complex was an controversial topic, however, recent research (Yang & Ishiguro, 2015 and references therein) suggested a dominance of cometary origin. In this study, we numerically investigated the orbital evolution of cometary dust particles, with special concerns on different evolutionary tracks and its consequences according to initial orbits, size and particle shape. The effect of dust particle density and initial size-frequency distribution (SFD) were not decisive in total cloud complex mass and mass supply rate, when these physical quantities are confined by observed zodiacal light brightness and dust particle SFD at 1 au. We noticed that, if we assume the existence of fluffy aggregates discovered in the Earth's stratosphere and the coma of 67P/Churyumov-Gerasimenko, the required mass supply rate decreases significantly. We also found out that close encounters with planets (mostly Jupiter) are the dominating factor of the orbital evolution of dust particles, as the result, the lifetime of cometary dust particles are shorter than Poynting-Robertson lifetime (around 250 thousand years). As another consequence of severe close encounters, only a small fraction of cometary dust particles can be transferred into the orbit < 1 au. This effect is significant for large size particles of ${\beta}$ < 0.01. The exceptional cases are dust particles ejected from 2P/Encke and active asteroids. Because they rarely encounter with Jupiter, most dust particles ejected from those objects are governed by Poynting-Robertson effect and well transferred into the orbits of small semimajor axis. In consideration of the above effects, we directly estimated probability of mutual collisions between dust particles and concluded that mutual collisions in the IDPs cloud complex is mostly ignorable, except for the case of large sized particles from active asteroids.

• Composites Research
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• 제36권3호
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• pp.230-240
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• 2023

전개형 반사판 안테나는 단위 구조물 형태의 반사판이 접힌 상태로 수납되어 발사체에 탑재된 후, 운용궤도에 도달 및 전개되어 임무를 수행하는 위성체이다. 전개형 반사판 안테나는 수납 부피를 줄일 수 있어 발사체의 제한적 수납공간에 대형 우주 구조물을 탑재시킬 수 있으며, 경량소재를 적용할 경우 발사 및 운용 성능 향상에 용이한 장점이 있다. 본 논문에서는 전개형 반사판 안테나를 구성하는 주반사판에 대해 강성 및 강도 등의 구조적 분석을 통해 초기 개념설계를 수행하였다. 탄소섬유 복합재 및 허니콤 코어를 적용하여 경량 복합재 주반사판을 설계하였으며, 적층 패턴 및 형상을 설계 변수로 운용조건에 적합한 주반사판 설계안을 도출하였다. 이후 모드(Modal analysis), 준정적(Quasi-static), 열 구배(Thermal gradient) 및 동적(Dynamic) 거동에 대한 상세 구조해석을 수행하여 경량 복합재 반사판 안테나의 성능을 분석하였다

• 천문학회보
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• 제45권1호
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• pp.46.3-47
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• 2020

Variations in the brightness of asteroids are caused by their spins, irregular shapes and companions. Thus, in principle, the spin state and shape model of a single object or, a combined model of spins, shapes and mutual orbit of a multiple components can be constructed from the analysis of light curves obtained from the time-series photometry. Using ground- and space-based facilities, a number of time-series photometric observations of asteroids have been conducted to find the possible causes of their light variations. Nonetheless, only about 2% of the known asteroids have been confirmed for their rotation periods. Therefore, a follow-on systematic photometric survey of asteroids is essential. We started an asteroid light curve survey for this purpose using Korea Microlensing Telescope Network (KMTNet) during 199 nights between the second half of 2019 and the first half of 2020. We monitored within a 2° × 14° region of the sky per each night with 25 min cadences. In order to observe as many asteroids as possible with a single exposure, we mostly focus on the ecliptic plane. In our survey, 25,925 asteroids were observed and about 8,000 of them were confirmed for their rotation periods. In addition, using KMTNet's 24-hour continuous monitoring, we collected many composite light curves of slow rotating asteroids that were rarely obtained with previous observations. In this presentation, we will introduce the typical light curves of asteroids obtained from our survey and present a statistical analysis of spin states and shapes of the asteroids from this study.

• 한국인터넷방송통신학회논문지
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• 제16권5호
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• pp.197-203
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• 2016

본 논문에서는 저궤도 소형위성에 탑재하여 빔 조향을 능동적으로 할 수 있는 다이폴 안테나를 설계하였다. 제안된 안테나는 야기-우다 안테나의 원리를 기반으로 하였으며, 2개의 무급전 기생소자를 T자형으로 형성시켜 수직소자의 길이를 고정시킨 후 수직소자의 끝단에서의 open, short에 따라 도파기 또는 반사기로 작동되게 하였다. 설계된 안테나는 UHF 대역의 436.5 MHz를 중심으로 위성-위성 간과 위성-지상 간의 링크버짓을 통해 안테나의 목표 이득을 정하였다. 안테나 특성을 향상시키기 위해 무급전 기생소자의 수직소자인 transformer의 길이를 변경시켰으며, transformer의 길이가 ${\lambda}/4$보다 ${\lambda}/2$일 때 최대 빔 방향 이득이 0.5 dB 향상되었다. 실제 ${\lambda}/2$ transformer 제작 시에는 무급전 기생 소자의 open, short를 다이오드와 캐패시터, 인덕터로 구성된 on/off switch를 이용하여 구현하였다. 그 결과 위성-위성 간 이득은 평균 5.92 dBi로 나타났으며 위상-지상 간 이득은 평균 0.99 dBi로 확인되어 링크버짓을 통해 정한 목표 스펙을 충분히 만족하였다.

• 한국자기학회지
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• 제25권2호
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• pp.52-57
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• 2015

텅스텐 타겟인 양극의 각도에 의존하는 X-선관 집속관의 전자빔 초점 크기를 오페라-3차원/스칼라(OPERA-3D/SCALAR) 프로그램을 이용하여 구하였다. 시뮬레이션 분석은 X-선관을 음극과 양극 그리고 4영역을 나누어 유한요소법을 적용하였다. X-선 집속관의 필라멘트로부터 방출되는 열전자 궤적은 전자밀도 분포함수에 따라 양극에 도달할 때 실초점으로 집속되고 양극에 부딪쳐서 유효 초점 크기로 X-선을 발생하게 된다. 전자빔 실초점 크기는 X-선 집속관 모양을 결정짓는 폭, 길이, 높이를 조절하여 줄일 수 있었고, 양극각도의 크기에 따라 미세하게 변하였다. 양극각도가 $10^{\circ}{\sim}17^{\circ}$에서는 전자빔 실초점 크기를 $70{\mu}m$ 이내로 유지하였고, 가장 최소 초점크기는 $15^{\circ}$에서 실초점 크기가 $40{\mu}m$로 나타났다. 최적화된 X-선 집속관의 변수들로 시뮬레이션하는 열전자의 방출 궤적을 분석하여 얻은 마이크로 크기인 실초점을 활용하는 새로운 의료 영상진단기기 개발이 가능할 것으로 보여진다.

• 대한방사선치료학회지
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• 제20권2호
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• pp.103-107
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• 2008

목적: 전자선 조사야에서 자기장의 유무, 세기와 형태에 따른 표면 선량의 변화를 알아보고 임상에서의 적용 가능성에 대하여 알아보고자 한다. 대상 및 방법: 6 MeV 전자선과 $10{\times}10\;cm^2$의 조사야를 이용하여 9개의 hole이 있는 차폐블록을 제작하여 필름 농도를 측정하고 전자선 조사야 내에 자장이 위치 할 때와 조사야의 외부에 위치 할 때의 선량변화를 필름과 표면선량 측정기를 이용하여 측정하였다. 결 과: 전자선의 입사각은 조사야의 중심에서 측면으로 4 cm 지점에서 3도 정도의 입사각을 나타내었으며, ring type의 자기장을 사용할 경우 0.9%의 표면선량 증가가 나타나고, lens block에 자기장을 위치시키면 1.58%의 표면선량이 증가하고, half 조사야의 중심 측면에 자기장을 위치시키면 조사야의 중심에 3.6%의 표면 선량 증가를 보였다. 결 론: 전자선은 선속의 중심에서 측면으로 일정 각도를 이루고 조사되어지며 자기장이 위치한 조사야내 표면선량의 변화는 자기장으로 인하여 전자선의 진행 방향이 변화되었음을 의미하고 안구와 같은 부위에 환자의 불편함이 없이 표면선량을 증가 시켜야 할 경우 유용한 방법으로 사용되어질 것이다.