• 한국항공우주학회지
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• 제43권5호
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• pp.387-395
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• 2015

초음속 흡입구의 부가항력을 계산하는 효율적인 방법을 개발하였으며 이 방법은 상용 유동 해석 소프트웨어인 STAR-CCM+을 사용한 유동 해석 결과를 이용한다. STAR-CCM+는 다면체 형상의 격자를 이용하여 효율적인 3차원 유동 해석을 수행할 수 있다. 세 가지 형상의 흡입구에 대해 두 가지의 유동 마하수와 여러 유량비 조건에 대한 해석을 수행하고 본 방법을 이용하여 부가항력을 계산하였으며 계산 결과를 풍동시험 결과와 비교하여 잘 일치하는 결과를 얻었다. 초임계 조건에 대한 초음속 흡입구 주위의 3차원 유동 해석은 비점성 가정을 사용하고 있지만, 점성 효과를 제외한 것이 부가항력 산출에 큰 영향을 주지 않은 것으로 사료되며 적은 격자와 단순한 경계조건의 사용이 가능하여 격자 생성과 유동 해석에 소요되는 노력과 시간의 절약으로 인해 효율적인 부가항력 산출에 기여했다고 판단된다.

• 천문학회보
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• 제38권1호
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• pp.32.1-32.1
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• 2013

We use numerical simulations to investigate the evolution of both the star formation rate (SFR) and the observable properties of equal-mass disk merger remnants for 18 different orbital configurations. In our analysis, the photometric properties of the remnants have been constructed by considering dust reddening effect in order to facilitate the comparison with observational data of large surveys such as the Sloan Digital Sky Survey (SDSS). First, we found that the detailed evolutions of merging galaxies are different between the merging characteristics such as merging time scale, SFR history, and burst efficiency. Around $70{\pm}5$ percent of gas turns into stars until the merger-induced starburst ends regardless of merger types. Our study also suggests that merger features involve a small fraction of stars. Merger features last roughly 3 times the final coalescence time of galaxy mergers. For a shallower surface brightness limit, the features seem to survive in a shorter time, which is the reason why detecting merger features by using shallow surveys were difficult in the past.

• 천문학회보
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• 제44권1호
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• pp.58.3-58.3
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• 2019

Optical intensity interferometry, developed in the 1950s, is a simple and inexpensive method for achieving angular resolutions on microarcsecond scales. Its low sensitivity has limited intensity interferometric observations to bright stars so far. Substantial improvements are possible by using avalanche photodiodes (APDs) as light detectors. We present here the results of laboratory measurements with a prototype astronomical intensity interferometer using APDs in continuous ("linear") detection mode - arguably, the first of its kind. We used two interferometer configurations, one with zero baseline and one with variable baseline. Using a superluminous diode as light source, we unambiguously detected Hanbury Brown-Twiss photon-photon correlations at very high significance. From measuring the correlation as function of baseline, we measured the angular diameter of the light source, in analogy to the measurement of the angular diameter of a star. Our results demonstrate the possibility to construct large astronomical intensity interferometers that can address a multitude of astrophysical science cases.

• International Journal of Naval Architecture and Ocean Engineering
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• 제12권1호
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• pp.468-478
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• 2020

The wave interaction problem with a vertical slotted breakwater, consisting of impermeable upper, lower parts and a permeable middle part, has been studied theoretically. An analytical model was presented for the estimation of reflection and transmission of monochromatic waves by a slotted breakwater. The far-field solution of the wave scattering involving nonlinear porous boundary condition was obtained using eigenfunction expansion method. The empirical formula for drag coefficient in the near-field, representing energy dissipation across the slotted barrier, was determined by curve fitting of the numerical solutions of 2-D channel flow using CFD code StarCCM+. The theoretical model was validated with laboratory experiments for various configurations of a slotted barrier. It showed that the developed analytical model can correctly predict the energy dissipation caused by turbulent eddies due to sudden contraction and expansion of a slotted barrier. The present paper provides a synergetic approach of the analytical and numerical modelling with minimum CPU time, for better estimation of the hydrodynamic performance of slotted breakwater.

• 한국정보처리학회논문지
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• 제1권4호
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• pp.427-437
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• 1994

스타형 컴퓨터 네트워크의 최적 부하균형 문제를 생각한다. 스타형 모델에서는 세가지 부하균형방향정책을 생각할 수 있다. 첫 번째는, 주변노드로 도착한 작업들은 자노드에서 처리되거나 자노드가 과부하인 경우 중앙노드에 보내져 처리될 수 있다. 두 번째는, 중앙노드에 도착한 작업만이 자노드에서 처리되거나 중앙노드가 과부하인 경우 저부하의 주변노드로 작업이 전송되어 처리될 수 있다. 본 연구에서는 두 번째 정책에 대하여 비선형 최적화 문제를 만들고, 최적해를 이용하여 최적 부가균형 알고 리즘을 제안한다. 세 번째는, 중앙노드 혹은 주변노드를 가리지 않고 도착한 작업들은 자노드에서 처리되거나 자노드가 과부하인 경우 저부하의 타노드로 작업이 전송되어 처리된다. 이 세 번째 부하균형 정책을 위한 부하분산 알고리즘도 제안한다. 본 논문 에서 대상으로 하고 있는 세가지 부하균형 정책을 수치실험을 통하여 비교분석 하였다. 수치실험 결과중 다음과 같은 몇 가지 재미있는 실험결과가 발견되었다. 세 번째 부하 균형 정책은 대부분의 경우 다른 두 정책보다 시스템 성능을 크게 향상시킨다. 두 번 째 부하균형 정책은 대부분의 경우 미약한 성능향상 밖에 보이지 않는다. 마지막으로 중앙노드의 처리능력이 주변노드보다 훨씬 큰 경우에는 첫 번째와 세 번째의 부하균 형 정책은 동일한 성능향상을 보인다.

• 천문학회보
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• 제45권1호
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• pp.42.2-42.2
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• 2020

We report on multi-wavelength observations of AA Ori, a Young Stellar Object in Orion-A star-forming region. AA Ori is known to have a pre-transitional disk based on infrared observations including Spitzer/IRS data. We construct its broadband spectral energy distribution (SED) by not only taking data in the optical and IR region but also including Herschel/PACS, JCMT/SCUBA, and SMA observational data. We use the Monte Carlo radiative transfer code (RADMC-3D) to reconstruct the SED with a viscous accretion disk model initialized by a radially continuous disk and finally having an inner and outer dusty disk separated by a dust-depleted radial gap. By comparing the model SEDs with different configurations of disk parameters, we discuss the limits to find a single solution of model parameters to fit the data. We suggest that some models with a modified inner disk surface density gradient and some degree of dust depletion in the inner disk can explain the AA Ori's SED, from which we infer that the inner disk of AA Ori has evolved. We present that model configurations of a pre-transitional disk with a large gap extended to 60-80 AU in a settled dusty disk of a few hundred AU size with a high inclination angle (~60°) also create model SEDs close to the observed one. To distinguish whether the disk has a just-opened narrow gap or a large gap, with an altered surface density of the inner disk extended to 10 AU, we suggest a further investigation of AA Ori with high angular resolution observations.

• 대한기계학회논문집B
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• 제41권6호
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• pp.373-380
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• 2017

본 연구에서는 레이놀즈 평균 나비어-스톡스(Reynolds-averaged Navier-Stokes, RANS) 방정식을 적용하여 스러스터(thruster) 상호작용에 대한 점성 유동 CFD 해석을 수행하였다. 수치해석은 상용 프로그램인 STAR-CCM+를 이용하였으며, 프로펠러와 No.19a 덕트로 스러스터 모델을 구성하였다. 프로펠러의 회전에 의한 동적인 움직임의 해석을 위해 슬라이딩 격자(sliding mesh)기법을 사용하였으며, 격자구성은 다중영역으로 구분하여 육면체 격자(hexahedral element)로 구성하였고, 계산 시간의 경제성을 고려하여 비등각(non-conformal) 격자를 이용하였다. 스러스터 배치를 그대로 유지한 상태에서 상류방향 스러스터의 방위각(azimuth angle)과 축 기울기에 따라 스러스터 상호작용이 크게 변화하였다. 이러한 결과를 통해 축 기울기와 방위각이 추진성능에 중요한 영향을 미치는 것을 확인하였다.

• 한국해양공학회지
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• 제28권5호
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• pp.378-386
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• 2014

In this study, the characteristics of the current and wind forces acting on two floating bodies were numerically investigated using a commercial CFD software, STAR-CCM+. In the numerical analyses, LNGC was located right behind FSRU under uniform current or wind conditions. Steady calculations were carried out using a Reynolds averaged Navier-Stokes (RANS) solver and the realized k-epsilon model. First, the current coefficients of FSRU based only the CFD were compared with the model test data. Through this comparison, the present numerical models and mesh systems were indirectly verified. Next, computations for FSRU and LNGC in a uniform current were performed using different relative positions. It was found that the current coefficients were great affected by the longitudinal positions. Finally, the wind forces acting on FSRU and LNGC in tandem configurations were studied. The focus was on the shielding effects due to the aerodynamic interactions between FSRU and LNGC.

• 천문학회보
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• 제42권2호
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• pp.37.1-37.1
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• 2017

Since the seminal work of Perrin, physicists have understood in the context of kinetic theory how ink slowly diffuses in a glass of water. The fluctuations of the stochastic forces acting on water molecules drive the diffusion of the ink in the fluid. This is the archetype of a process described by the so-called fluctuation-dissipation theorem, which universally relates the rate of diffusion to the power spectrum of the fluctuating forces. For stars in galaxies, a similar process occurs but with two significant differences, due to the long-range nature of the gravitational interaction: (i) for the diffusion to be effective, stars need to resonate, i.e. present commensurable frequencies, otherwise they only follow the orbit imposed by their mean field; (ii) the amplitudes of the induced fluctuating forces are significantly boosted by collective effects, i.e. by the fact that, because of self-gravity, each star generates a wake in its neighbours. In the expanding universe, an overdense perturbation passing a critical threshold will collapse onto itself and, through violent relaxation and mergers, rapidly converge towards a stationary, phase-mixed and highly symmetric state, with a partially frozen orbital structure. The object is then locked in a quasi-stationary state imposed by its mean gravitational field. Of particular interests are strongly responsive colder systems which, given time and kicks, find the opportunity to significantly reshuffle their orbital structure towards more likely configurations. This presentation aims to explain this long-term reshuffling called gravity-driven secular evolution on cosmic timescales, described by extended kinetic theory. I will illustrate this with radial migration, disc thickening and the stellar cluster in the galactic centre.

• 천문학회지
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• 제31권1호
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• pp.27-37
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• 1998

We have made semi-analytical studies to investigate the configurations of caustics and the probability distribution of the flux factor K for the binary microlensing including external shears. A parametric equation of critical curve is derived in a 4th order complex polynomial. We present the topological dependencies of the caustics for selected gamma parameters (0, 0.3, 0.6, 1.3, 2.0, and 2.5) and convergence terms (0., 0.4, 0.8, 1.2, 1.6, and 2.0). For the purpose of analyzing the efficiency of High Amplification Event (HAE) on each caustics, we examine the probability distribution of the flux factor by a Monte Carlo method. Changing the separation of the binary system from 0.8 to 1.3 (in normalied unit), we examine the probability distribution of the K-values in various gamma parameters. The relationship between gamma parameters, seperations and their probabilties of the flux factor K have been studied. Our results show that the relatively higher K values (K>1.5) are increased as increasing the separation of the binary system. We therfore conclude that, in the N-body microlensing, the probabilities of higher HAEs are inversely proportional to the star density as well. We also point out that the present research might be used as a preliminary step toward investigating heavy N-body microlensing simulations.