• Wind and Structures
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• 제5권2_3_4호
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• pp.337-346
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• 2002

Wind tunnel pressure measurements and numerical simulations based on the Reynolds Stress Model (RSM) are compared with full and model scale data in the flow area of impingement, separation and wake for $60^{\circ}$ and $90^{\circ}$ wind azimuth angles. The phase averaged fluctuating pressures simulated by the RSM model are combined with modelling of the small scale, random pressure field to produce the total, instantaneous pressures. Time averaged, rsm and peak pressure coefficients are consequently calculated. This numerical approach predicts slightly better the pressure field on the roof of the TTU (Texas Tech University) building when compared to the wind tunnel experimental results. However, it shows a deviation from both experimental data sets in the impingement and wake regions. The limitations of the RSM model in resolving the intermittent flow field associated with the corner vortex formation are discussed. Also, correlations between the largest roof suctions and the corner vortex "switching phenomena" are observed. It is inferred that the intermittency and short duration of this vortex switching might be related to both the wind tunnel and numerical simulation under-prediction of the peak roof suctions for oblique wind directions.

• Structural Engineering and Mechanics
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• 제10권3호
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• pp.245-262
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• 2000

The objective of this study is to analyze the deformational characteristics of a high-vacuum insulation panel that is evacuated to eliminate significant gas-phase conductance through its thickness. The panel is composed of a metal envelope and low thermal conductance spacers. The problem is very challenging because several nonlinearities are involved concurrently. Not only are various finite element models such as triangular, rectangular, beam and circular plate models used to simulate the panel, but also several finite element programs are used to solve the problem based on the characteristics of the finite element model. The numerical results indicate that the effect of the diameter of the spacer on the vertical deformation of the plate panel is negligibly small. The parameter that mainly influences the maximum sag is the spacing between the spacers. The maximum vertical deformation of the panel can be predicted for a practical range of the spacing between the spacers and the thickness of the plate. Compared with the numerical results obtained by the finite element models and the experimental tests, they have a good agreement. The results are represented in both tabular and graphical forms. In order to make the results useful, a curve fitting technique has been applied to predict the maximum deformation of the panel with various parameters. Moreover, the panel was suggested to be a "smart" structure based on thermal effect.

• 천문학논총
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• 제15권spc1호
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• pp.93-102
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• 2000

We have reviewed the magnetic activity in close binaries. Solar like magnetic activity indicators such as photometric spots, chromo spheric emission, coronal X-ray and radio emission, and flare activity are commonplace in many cool stars with convective envelopes. Using the UV spectra we confirmed the strength of stellar activity increases with more rapid rotation and later spectral types which corresponds to the increasing depth of the star's convective envelope. Apart from very young stellar objects such as T Tauri stars, the stars with the highest levels of activity are close binary systems composed of cool stars, i.e., the chromospherically active binaries such as RS CVn, BY Dra, W UMa and related systems. The IUE low and high dispersion spectra of V711 Tau, VW Cep and SW Lac are used for ultraviolet photometry and for a variation study of chromospheric activity. Evidence of chromospherically activity is indicated by the intensity variation of the Mg II emission line with orbital phase.

• 천문학회보
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• 제37권1호
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• pp.55.2-55.2
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• 2012

Silicate-carbon stars are characterized by oxygen-rich (O-rich) dust features despite their carbon-rich (C-rich) photospheres. While the origin of silicate-carbon stars has been a mystery ever since their discovery, the most widely accepted hypothesis is that the silicate-carbon stars have a low-luminosity companion and the O-rich material is stored in a circumbinary disk or a circumstellar disk even after the primary star becomes a carbon star. In order to study the properties of circumstellar dust envelopes of silicate-carbon stars, we perform radiative transfer model calculations using RADMC-3D with an axi-symmetric dust density distribution (a disk) as well as a spherically symmetric dust distribution. For various dust envelope models with different shapes and chemistry, we calculate the model spectral energy distributions (SEDs) and compare the model results with the observed SEDs of selected 5 silicate-carbon stars. The Circumstellar disk models are fairly well fitted with the observational data of 5 silicate-carbon stars. We find some evidences that the circumbinary disk model could be a better explanation for the origin of silicate carbon stars than the simple detached silicate dust shell model of the transition phase of the stellar chemistry.

• 한국전자파학회지:전자파기술
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• 제5권3호
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• pp.22-35
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• 1994

본 논문에서는 대역폭 효율의 향상을 위해 상관 부호에 따른 FM시스템올 설계한다. 상판 부호화된 신호는 연속 위상과 정진폭 특성으로 전력 효율이 높다. 하지만 이 신호는 최소 유콜리언 거리(${d^2}_{mm}$)가 작기 때분에 신호대 잡음비(SNR)의 손실과 수신 성능(BER)의 저하를 초래한다. 따라서 본 논문에서는 수신 성능의 향상을 위하여 상관 부호화에 따른 수정된 최대 근사 추정을 작용한다. 최대 근사 추정은 사용된 채널에서 bit-by-bit 검파에 비하여 수산 오율을 향상시킨다. 결정 궤환을 적용하지 않은 경우, 최대 근사 추정은 bit by bit 겁파에 비해 약 2dB의 수신 성능이 향상되었다. 결정 궤환을 적용한 경우, 최대 근사 추정은 bit-by bit 검파에 비해 약 4dB의 수신 성능이 향상되었다. 특히 안정된 채널보다 채널이 열악할수록 최대 근사 추정과 결정 궤환의 성능이 우수하다.

• 한국재료학회지
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• 제13권10호
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• pp.651-657
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• 2003

Ultrasonic microscope has been used to detect the defects on surface or inner solid. Conventionally, it has used at a single operating frequency. The resolution and quality of the measured images are determined by a characteristic of the transducer of the ultrasonic microscope. The conventional ultrasonic microscope has been used envelope detector to detect the amplitude of reflected signal, but the changes in amplitude is not sensitive enough for specimen with microstructure that in phase. In this paper, we have studied multi-frequency depth resolution enhancement with ultrasonic reflection microscope for the reflectors of a stainless steel reference specimen and a reference calibration block to be used as the material in nuclear power plants for ISI, PSI. Increased depth resolution can be obtained by taking two, three-dimensional images at more that one frequency and numerically combining the results. As results of the experiment, we could get enhanced images with the rate of contrast in proportion and high quality signal distribution for the image to the changing rate of depth for the reflectors of the two kinds of specimens.

• 한국통신학회논문지
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• 제16권5호
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• pp.413-423
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• 1991

3RC, 3SRC, 4SRC, TFM등과 같은 몇몇 디지틀 PRCPM 신호는 정 진폭 특성과 밀집된(Compact) 전력 스펙트럼을 갖는다. 그러나 페이딩하에서 단순한 주파수 검파를 사용했을 때 이들의 BER은 너무 높다. 이는 근접 비트들 때문에 생기는 높은 ISI에 기인한다. 본 논문에서는 하나의 근접 비트 때문에 생기는 ISI 재기를 위해 DFE(Decision Feedback Equalization)을 사용하였고, 이때의 BER 성능 향상을 이론적으로 살펴보았다. 또한, DEF를 사용한 경우와 사용하지 않은 경우의 BER 성능 비교를 위해 수치 결과들을 제시하였다.

• 한국추진공학회:학술대회논문집
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• 한국추진공학회 2003년도 제20회 춘계학술대회 논문집
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• pp.225-232
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• 2003

분리 삼중충돌 제트의 액상 혼합에 대한 실험적 연구결과를 통해 분리 삼중충돌 인젝터의 요소설계시 고려해야 할 기하학적 파라메타와 혼합성능을 고려하는 방법을 제시하였다. 실험은 비반응성인 케로신과 물을 사용하여 수행하였으며, 분사공의 기학적 조건과 분사조건(운동량비)에 따른 국소혼합비 분포를 측정하여 혼합효율 및 혼합특성속도를 산출하였다. 분사공의 각종 기하학적 요소와 운동량비에 따른 혼합효율 및 혼합 특성속도를 비교/분석하고 혼합성능과 연소성능과의 상관관계를 규명하였으며, 혼합의 정도를 향상시키는 설계점과 혼합성능 측면에서의 분리 삼중충돌 인젝터의 최적 설계조건에 대하여 고찰하였다.

• 천문학회보
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• 제41권1호
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• pp.77.4-78
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• 2016

Binary interactions may have significant impact on Pop III stellar evolution. Pop III single star evolution indicates that for primary masses less than $20M_{\odot}$, no significant binary mass transfer would occur before core helium exhaustion. We perform binary system evolution for various primary masses ($20M_{\odot}$ < $M_1$ < $60M_{\odot}$) and initial periods under same mass ratio $M_2/M_1=0.9$, and follow the evolution and mass transfer of the primary star. If binary mass transfer occurs during post main sequence, the primary star does not evolve into naked helium star and still contain significant hydrogen in the envelope. During the post mass transfer phase, the primary star evolves redward, and does not become sufficiently hot to enhance the number of ionizing photons, compared to the case of single star evolution for a given initial mass. This result implies that primary stars of massive Pop III binary systems would have little contribution to the reionization in the early universe. Given the large hydrogen content ($0.326-1.793M_{\odot}$), the primary stars that underwent stable mass transfers would explode as a Type IIb supernova, and it would be difficult for Pop III binary stars to produce Type Ib/c supernovae that look similar to those found in the local universe.

• 대한전기학회:학술대회논문집
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• 대한전기학회 2004년도 추계학술대회 논문집 전기물성,응용부문
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• pp.281-284
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• 2004

In Recent, it became necessary to envelope the technology about electrodeless fluorescent lamp according to demand of the electrodeless fluorescent lamp system that used higher efficiency and advantage of long-lifetime. Especially, in the electrodeless fluorescent lamp which used H-mode, efficiency of lamp is decided from matching parameter of antena and inverter So it is of the utmost importance to design antena and inverter. Therefore, this paper used a transformer principle for efficiency rising of electrodeless fluorescent lamp and interpreted an equivalent circuit, used an impedance analyzer in order to confirm a performance enhancement of lamp along design of antenna, and confirmed parameter characteristic of R, L, C, Z, Phase, Q-factor along a change of magnetic flux density. Also, this paper confirmed a luminance characteristic of electrodeless lamp along parameter change with measuring optical characteristic along a change of magnetic flux density.