• Journal of Astronomy and Space Sciences
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• 제27권2호
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• pp.89-96
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• 2010

BVR CCD observations of GW Cep were made on 15 nights in November through December 2008 with a 1-m reflector at the Jincheon station of the Chungbuk National University Observatory. Nineteen new times of minimum lights for GW Cep were determined and added to a collection of all other times of minima available to us. These data were then intensively analyzed, by reference to an O-C diagram, to deduce the general form of period variation for GW Cep. It was found that the O-C diagram could be interpreted as presenting two different forms of period change: an exclusively quasi-sinusoidal change with a period of 32.6 years and an eccentricity of 0.10; and a quasi-sinusoidal change with a period of 46.2 years and an eccentricity of 0.36 superposed on an upward parabola. Although a final conclusion is somewhat premature at present, the latter seems more plausible because late-type contact binaries allow an inter-exchange of both energy and mass between the component stars. The quasi-sinusoidal characteristics were interpreted in terms of a light-time effect due to an unseen tertiary component. The minimum masses of the tertiary component for both cases were calculated to be nearly the same as the $0.23-0.26M\;{\odot}$-ranges which is hardly detectable in a light curve synthesis. The upward parabolic O-C diagram corresponding to a secular period increase of about $4.12{\times}10^{-8}\;d/yr$ was interpreted as mass being transferred from the lesser to more massive component. The transfer rate for a conservative case was calculated to be about $2.66\;{\times}\;10^{-8}\;M_{\odot}/yr$ which is compatible with other W UMa-type contact binaries.

• 대한전자공학회논문지TC
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• 제46권3호
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• pp.32-39
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• 2009

본 논문은 초광대역 임펄스를 이용한 지반탐사 영상레이더 시스템 (Ground Penetrating Image Radar; GPIR) 설계에서 수직심도의 해상도를 높이기 위한 시간영역 관점에서의 최적화 설계방법을 제시하였다. 시스템의 핵심 부분인 임펄스 발생원 및 초광대역 안테나에 대하여 시간영역에서의 해석 기법을 제시하였고, 시뮬레이션에 의해 최적 설계 파라미터를 설정하였다. 특히, 임펄스 신호의 파형을 정형화하여 임펄스 신호의 스펙트럼 효율을 높였으며, 초광대역 안테나로는 U자형 평판형 다이폴 안테나를 사용하였다. 제안된 안테나는 반사체를 사용하여 외부 잡음을 차단하였고, 지중과의 신호 결합을 개선하였다. 또한 시스템의 성능을 열화시키는 안테나에 의한 떨림을 제거하기 위해, 저항을 사용하였고, 송수신 안테나는 시간영역 시뮬레이션을 통하여 최적화 하였다. 지중 매질의 영상화를 위해 마이그레이션을 기법을 사용하였으며, 지면의 영향 등에 의한 수신된 펄스의 왜곡 현상은 시간영역에서의 잡음 및 신호 왜곡 저감 기법을 사용하여 성능을 개선하였다. 최적화된 설계 방법의 평가를 위하여, 지중 매설물 탐지용 레이더 시제품을 개발하였고, 성능 시험을 위한 시험장을 활용하였다. 측정 결과 수직 심도는 이론적 인 해 상도만큼 우수한 성능을 보였다.

• 대한설비공학회:학술대회논문집
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• 대한설비공학회 2007년도 동계학술발표대회 논문집
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• pp.570-575
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• 2007

The thermal performance of the air receiver filled with porous material for 5kWt dish solar collector installed in Inha University, Korea, is experimentally investigated. The diameter of the parabolic dish is 3.2 m, and its focal length is 2 m. It consists of 10 small pieces of glasses which have their own curvatures, and the effective reflecting area is 5.9 m2. The reflectivity of the glass is 0.95, and the thermal capacity of the system is about 5 kW thermal. The aperture diameter of the cylindrical-shape receiver which is made of stainless steel is 100 mm, and the height is 210 mm. A quartz window is installed at the receiver aperture to minimize the convective heat loss and prevent air leakages. In order to increase the heat transfer area, porous material (nickel-alloy) is inserted into the receiver. Air flows into the upper part of the receiver, which is the opposite side of the aperture. After the air flows through the inside receiver, that goes out of the receiver through 3 exits which are located near the aperture. The volumetric flow rates of air are varied from 600 to 1200 L/min. The thermal efficiency of the receiver ranges from 82% - 92% depending upon the flow rate. The results show that the system efficiency and receiver efficiency increase as the volume flow rate increases as expected. These results from the experiment will be useful for the applications to air heating receivers and solar reactors.