• 대한조선학회지
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• 제19권1호
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• pp.23-32
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• 1982

Herein the motion of a freely-floating sphere in a water of finite depth is analysed within the framework of a linear potential theory. A velocity potential describing fluid motion is generated by distributing pulsating sources and dipoles on the immersed surface of the sphere, without introducing an inner flow model. The potential becomes the solution of an integral equation of Fredholm's second type. In the light of the vertical axisymmetry of the flow, surface integrals reduce to line integrals, which are approximated by summation of the products of the integrand and the length of segments along the contour. Following this computational scheme the diffraction potential and the radiation potential are determined from the same algorithm of solving a set of simultaneous linear equations. Upon knowing values of the potentials hydrodynamic forces such as added mass, hydrodynamic damping and wave exciting forces are evaluated by the integrating pressure over the immersed surface of the sphere. It is found in the case of finite water depth that the hydrodynamic forces are much different from the corresponding ones in deep water. Accordingly motion response of the sphere in a water of finite depth displays a particular behavior both in a amplitude and phase.

• Structural Engineering and Mechanics
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• 제85권4호
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• pp.445-459
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• 2023

The current investigation is the first endeavor to apply the full layerwise finite element method (FEM) in free vibration analysis of functionally graded (FG) composite plates reinforced with graphene nanoplatelets (GPLs) in thermal environment. Unlike the equivalent single-layer (ESL) theories, the layerwise FEM focuses on all three-dimensional (3D) effects. The GPLs weight fraction is presumed invariable in each layer but varies through the plate thickness in a layerwise model. The modified Halpin-Tsai model is employed to acquire the effective Young's modulus. The rule of mixtures is applied to specify the effective Poisson's ratio and mass density. First, the current method is validated by comparing the numerical results with those stated in the available works. Next, a thorough numerical study is performed to examine the influence of various factors involving the pattern of distribution, weight fraction, geometry, and size of GPLs, together with the thickness-to-span ratio, thermal environment, and boundary conditions of the plate, on its free vibration behaviors. Numerical results demonstrate that employing a small percentage of GPL as reinforcement considerably grows the natural frequencies of the pure epoxy. Also, distributing more square-shaped GPLs, involving a smaller amount of graphene layers, and vicinity to the upper and lower surfaces make it the most efficient method to enhance the free vibration behaviors of the plate.

• 한국가스학회지
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• 제22권6호
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• pp.16-27
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• 2018

대한민국 정부에서 2014년부터 LPG배관망과 LPG소형탱크를 도시가스 공급망 개설이 어려운 산간이나 도서지역에 보급하는 사업을 시작했다. 마을단위와 군단위로 LPG집단공급시설을 설치하면서 기존의 가스공급 압력이 아닌 10배 이상의 높은 준저압(25kPa~100kPa)으로 소비자에게 공급하게 되면서 가스사고의 위험성이 높아졌다. 기존의 가스공급압력보다 10배 이상 높은 압력이기 때문에 가스가 누출 되었을 때 빠른 속도로 많은 양이 누출하게 된다. 이에 준저압 가스배관의 안전성 확보를 위해 과류차단밸브가 필요하게 되었지만, 국내에서는 준저압 매몰배관용 과류차단밸브가 미개발되어 있으며 보급 또한 되어 있지 않는 상황이다. 이에 한국가스안전공사에서는 과류차단밸브의 국산화를 위해 과류차단밸브를 기개발한 해외의 성능기준과 제품을 조사 중에 있으며, 과류차단밸브의 성능평가를 위해 성능시험설비를 구축하여 준저압 연료가스 매몰배관용 과류차단밸브를 연구 개발 중에 있다.

• 한국응용곤충학회지
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• 제60권3호
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• pp.287-304
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• 2021

우리나라의 천적 연구는 1995년부터 본격적으로 추진되었다. 25여 년이 지난 지금 1990년부터 2020년까지 한국응용곤충학회지에 발표된 논문은 약 130편으로 전체 약 1,550편의 8.4%가 천적에 관한 논문이었다. 이들 논문 중에는 1990년대에는 천적을 탐색하여 생물적 특성 연구에 관한 논문의 비율이 높았고, 2010년대에는 개발된 천적을 농가 현장에 적용하는 논문의 비율이 높았다. 이러한 연구의 결과로 국내 토착 천적이 24종, 도입 천적이 13종이 개발되어 총 37종의 우수 천적이 개발되었다. 또한 개발된 천적이 현장에 활용될 수 있도록 천적 활용 기술서 및 매뉴얼을 약 28종 이상 개발되었다. 이처럼 지금까지 천적 탐색, 생물적 특성 연구, 및 생산·이용 기술 측면에서 많은 성과가 있었으나 앞으로 추진하여야 할 과제도 많이 남아 있다. 우리나라 농작물 재배상황에 맞는 우수 천적을 탐색하거나 도입하는 연구, 비용을 절감할 수 있는 연중 대량생산 기술, 천적의 생산 및 유통 과정에 품질을 유지할 수 있는 기술, 및 천적과 저독성 작물보호제를 조화롭게 사용할 수 있는 기술 개발 등이 필요할 것으로 생각된다.

• 천문학회지
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• 제47권6호
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• pp.235-253
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• 2014

Intensity interferometry, based on the Hanbury Brown-Twiss effect, is a simple and inexpensive method for optical interferometry at microarcsecond angular resolutions; its use in astronomy was abandoned in the 1970s because of low sensitivity. Motivated by recent technical developments, we argue that the sensitivity of large modern intensity interferometers can be improved by factors up to approximately 25 000, corresponding to 11 photometric magnitudes, compared to the pioneering Narrabri Stellar Interferometer. This is made possible by (i) using avalanche photodiodes (APD) as light detectors, (ii) distributing the light received from the source over multiple independent spectral channels, and (iii) use of arrays composed of multiple large light collectors. Our approach permits the construction of large (with baselines ranging from few kilometers to intercontinental distances) optical interferometers at the cost of (very) long-baseline radio interferometers. Realistic intensity interferometer designs are able to achieve limiting R-band magnitudes as good as $m_R{\approx}14$, sufficient for spatially resolved observations of main-sequence O-type stars in the Magellanic Clouds. Multi-channel intensity interferometers can address a wide variety of science cases: (i) linear radii, effective temperatures, and luminosities of stars, via direct measurements of stellar angular sizes; (ii) mass-radius relationships of compact stellar remnants, via direct measurements of the angular sizes of white dwarfs; (iii) stellar rotation, via observations of rotation flattening and surface gravity darkening; (iv) stellar convection and the interaction of stellar photospheres and magnetic fields, via observations of dark and bright starspots; (v) the structure and evolution of multiple stars, via mapping of the companion stars and of accretion flows in interacting binaries; (vi) direct measurements of interstellar distances, derived from angular diameters of stars or via the interferometric Baade-Wesselink method; (vii) the physics of gas accretion onto supermassive black holes, via resolved observations of the central engines of luminous active galactic nuclei; and (viii) calibration of amplitude interferometers by providing a sample of calibrator stars.