• Proceedings of the Korea Water Resources Association Conference
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• 2009.05a
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• pp.2033-2037
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• 2009

호소내의 흐름은 중력의 영향을 받는 하천의 흐름과는 달리 열수지에 의한 밀도류 및 바람 등에 영향을 크게 받아 특유의 유동특성을 나타낸다. 본 연구에서는 EFDC(Environmental fluid Dynamics Code, 미국 버지니아 해양연구소 개발) 모델을 이용하여 호소 내 수치모의를 실시하였다. 복잡한 지형을 형성하고 있는 호수 내의 유동특성의 정밀도를 향상시키기 위해서는, 흐름특성을 고려한 grid작성이 중요하다. 본 연구에서는 1:3000, 1:5000 축척의 수치지도를 이용하여 장흥호의 하상단면 값을 추정하였으며, GIS를 이용하여 (${\Delta}x$, ${\Delta}y$)=100m로 DEM을 생성하였다. 그리고 구성된 DEM값을 이용하여 정밀도가 높은 최종 Cartesian grid(active cell=706)를 구축하였다. EFDC를 이용한 장흥호의 수치모의 결과 호수내의 흐름은 수면을 통한 열 교환에 의한 수온 밀도류를 형성하고 있으며, 수온성층의 형성과 파괴가 호수 흐름을 형성하는 큰 인자로 작용한다는 것을 확인할 수 있었다. 그리고, 호에 유입되는 하천부분에서는 유입되는 수온에 따라 흐름특성이 변하며, 유입수온에 따라 호수 내 관입위치가 변하여 표면흐름, 내부흐름, 저부흐름 등의 흐름특성을 보인다 이상과 같이, 호수내의 흐름특성을 열수지, 외력에 의해서 크게 변동하며 해석대상역의 지역특성을 반영한 수리현상의 정확한 재현 없이는, 이 유동해석결과를 입력치로 하는 수질모델링 결과는 신뢰도에 심각한 문제를 발생시킨다고 할 수 있다.

• The Bulletin of The Korean Astronomical Society
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• v.42 no.2
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• pp.44.1-44.1
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• 2017

In barred galaxies, gaseous structures such a nuclear ring and dust lanes are formed by a non-axisymmetric stellar bar potential, and the evolution of the stellar bar is influenced by mass inflows to the center and central star formation. To study how the presence of the gas affects the evolution of the stellar bar, we use the mesh-free hydrodynamics code GIZMO and run fully self-consistent three-dimensional simulations. To explore the evolution with differing initial conditions, we vary the fraction of the gas and stability of initial disks. In cases when the initial disk is stable with Q=1.2, the bar strength in the model with 5% gas is weaker than that in the gas-free model, while the bar with 10% gas does not form a bar. This suggests that the gaseous component is unfavorable to the bar formation dynamically. On the other hand, in models with relatively unstable disk with Q=1.0, the presence of gas helps form a bar: the bar forms more rapidly and strongly as the gas fraction increases. This is because the unable disks form stars vigorously, which in turn cools down the stellar disk by adding newly-created stars with low velocity dispersion. However, the central mass concentration also quickly increases as the bar grows in these unstable models, resulting in fast bar dissolution in gas rich models. We will discuss our results in comparison with previous work.

• Journal of The Korean Astronomical Society
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• v.48 no.2
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• pp.139-154
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• 2015

We carry out three-dimensional hydrodynamic simulations of the supernova remnants (SNRs) produced inside molecular clouds (MCs) near their surface using the HLL code (Harten et al. 1983). We explore the dynamical evolution and the X-ray morphology of SNRs after breaking through the MC surface for ranges of the explosion depths below the surface and the density ratios of the clouds to the intercloud media (ICM). We find that if an SNR breaks out through an MC surface in its Sedov stage, the outermost dense shell of the remnant is divided into several layers. The divided layers are subject to the Rayleigh-Taylor instability and fragmented. On the other hand, if an SNR breaks through an MC after the remnant enters the snowplow phase, the radiative shell is not divided to layers. We also compare the predictions of previous analytic solutions for the expansion of SNRs in stratified media with our onedimensional simulations. Moreover, we produce synthetic X-ray surface brightness in order to research the center-bright X-ray morphology shown in thermal composite SNRs. In the late stages, a breakout SNR shows the center-bright X-ray morphology inside an MC in our results. We apply our model to the observational results of the X-ray morphology of the thermal composite SNR 3C 391.

• The Bulletin of The Korean Astronomical Society
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• v.41 no.1
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• pp.50.2-50.2
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• 2016

Continuous accretion of metal-poor gas can explain the discrepancy between the number of observed G-dwarfs and the number predicted by the "simple model" of galactic evolution. The maximum accretion rate estimated based upon approaching high velocity clouds (HVCs) can be up to ${\sim}0.4M_{\odot}{\cdot}yr^{-1}$ which is comparable with the accretion rate required by many chemical evolution models that is at least ${\sim}0.45M_{\odot}{\cdot}yr^{-1}$. However, it is not clear to what extent the exchange of gas between the disk and the cloud can occur when an HVC collides with the galactic disk. Therefore, we examined a series of HVC-Disk collision simulations using the FLASH 2.5 hydrodynamics simulation code. The outcomes of our simulations show that an HVC will more likely take away substances from the galactic disk rather than adding new material to the disk. We define this as an HVC having a "negative fuel rate". Further results in our study also indicate that the process and amount of fuel rate change can have various forms depending on the density, radius and velocity of an approaching HVC. The simulations in our study covers HVCs with a neutral hydrogen volume density from $1.0{\times}10^{-2}cm^{-3}$ to $41.0cm^{-3}$, radius of 200 pc to 1000 pc and velocity in the range between $40km{\cdot}s^{-1}$ and $100km{\cdot}s^{-1}$.

• Publications of The Korean Astronomical Society
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• v.30 no.2
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• pp.113-114
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• 2015

Recent high-resolution, high-sensitivity observations of protostellar jets have shown many to possess an underlying 'wiggle' structure. HH 211 is one such example where recent sub-mm observations revealed a clear reflection-symmetric wiggle. An explanation for this is that the HH211 jet source is moving as part of a protobinary system. Here we test this assumption by simulating HH211 through 3D hydrodynamic simulations using the pluto code with a molecular chemistry and cooling module, and initial conditions based on an analytical model derived from SMA observations. Molecular chemistry allows us to accurately plot synthetic molecular emission maps and position-velocity diagrams for direct comparison to observations, enabling us to test the observational assumptions and put constraints on the physical parameters of HH211. Our preliminary results show that the reflection-symmetric wiggle can be recreated through the assumption of a jet source being part of a binary system.

• Journal of Korea Society of Waste Management
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• v.34 no.7
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• pp.685-696
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• 2017

This study focuses on computational particle fluid dynamics (CPFD) modeling for the fast pyrolysis of biomass in a conical spouted bed reactor. The CPFD simulation was conducted to understand the hydrodynamics, heat transfer, and biomass fast pyrolysis reaction of the conical spouted bed reactor and the multiphase-particle in cell (MP-PIC) model was used to investigate the fast pyrolysis of biomass in a conical spouted bed reactor. A two-stage semi-global kinetics model was applied to model the fast pyrolysis reaction of biomass and the commercial code (Barracuda) was used in simulations. The temperature of solid particles in a conical spouted bed reactor showed a uniform temperature distribution along the reactor height. The yield of fast pyrolysis products from the simulation was compared with the experimental data; the yield of fast pyrolysis products was 74.1wt.% tar, 17.4wt.% gas, and 8.5wt.% char. The comparison of experimental measurements and model predictions shows the model's accuracy. The CPFD simulation results had great potential to aid the future design and optimization of the fast pyrolysis process for biomass.

• Journal of the Korean Society for Aeronautical & Space Sciences
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• v.50 no.12
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• pp.829-838
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• 2022

This study conducts Hypervelocity Impact(HVI) simulations considering space objects with various shapes and different impact angles. A commercial nonlinear structural dynamics analysis code, LS-DYNA, is used for the present simulation study. The Smoothed Particle Hydrodynamic(SPH) method is applied to represent the impact phenomena with hypervelocity. Mie-Grüneisen Equation of State and Johnson-Cook material model are used to consider nonlinear structural behaviors of metallic materials. The space objects with various shapes are modeled as a sphere, cube, cylinder, and cone, respectively. The space structure is modeled as a thin plate(200 mm×200 mm×2 mm). HVI simulations are conducted when space objects with various shapes with 4.119 km/s collide with the space structures, and the impact phenomena such as a debris cloud are analyzed considering the space objects with various shapes having the same mass at the different impact angles of 0°, 30° and 45° between the space object and space structure. Although space objects have the same kinetic energy, different debris clouds are generated due to different shapes. In addition, it is investigated that the size of the debris cloud is decreased by impact angles.

• Journal of The Korean Astronomical Society
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• v.35 no.4
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• pp.159-174
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• 2002

Cosmological hydrodynamic simulations of large scale structure in the universe have shown that accretion shocks and merger shocks form due to flow motions associated with the gravitational collapse of nonlinear structures. Estimated speed and curvature radius of these shocks could be as large as a few 1000 km/s and several Mpc, respectively. According to the diffusive shock acceleration theory, populations of cosmic-ray particles can be injected and accelerated to very high energy by astrophysical shocks in tenuous plasmas. In order to explore the cosmic ray acceleration at the cosmic shocks, we have performed nonlinear numerical simulations of cosmic ray (CR) modified shocks with the newly developed CRASH (Cosmic Ray Amr SHock) numerical code. We adopted the Bohm diffusion model for CRs, based on the hypothesis that strong Alfven waves are self-generated by streaming CRs. The shock formation simulation includes a plasma-physics-based 'injection' model that transfers a small proportion of the thermal proton flux through the shock into low energy CRs for acceleration there. We found that, for strong accretion shocks, CRs can absorb most of shock kinetic energy and the accretion shock speed is reduced up to $20\%$, compared to pure gas dynamic shocks. For merger shocks with small Mach numbers, however, the energy transfer to CRs is only about $10-20\%$ with an associated CR particle fraction of $10^{-3}$. Nonlinear feedback due to the CR pressure is insignificant in the latter shocks. Although detailed results depend on models for the particle diffusion and injection, these calculations show that cosmic shocks in large scale structure could provide acceleration sites of extragalactic cosmic rays of the highest energy.

• Proceedings of the Korea Water Resources Association Conference
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• 2009.05a
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• pp.2220-2224
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• 2009

하천의 수질모의를 위해서는 정상상태 모델인 QUAL2E 가 널리 사용되어 왔다. 그러나 우리나라는 기후 특성상 하절기에 강우가 집중되고 경우에 따라서는 댐등에 의해 장기간 수류의 지체현상이 발생하므로 지역 및 시기에 따라 발생하는 수질 문제가 서로 다를 수 있다. 따라서 우리나라의 대부분의 수체에서는 시간에 따라 모의를 할 수 있는 비정상 상태의 수질모델이 적용되어야 할 필요가 종종 발생한다. 미국공병단에서 개발된 CE-QUAL-W2 모델은 2차원 모델로서 수리동역학과 수질반응역학을 한데 묶어서 풀이하였다는 점에서 획기적인 변화로 볼 수 있다. 이 모델은 종방향으로 길고 수심이 깊으며 상대적으로 하폭이 좁은 형태의 수체에 적합하며 하폭방향의 수질 변화를 나타내는 데 사용되지 못하는 단점이 있다. WASP(Water Quality Analysis and Simulation Program) 은 미국 환경부에서 개발한 비정상상태 3차원 수질모델로서 세계적으로 다양한 수체에 널리 사용되어 왔다. 이 모델에서 1차원적 흐름을 예측할 수 있는 DYNHYD 라는 수리학적 부프로그램은 2차원 또는 3차원 상황에서는 사용할 수가 없었음에 따라 수리학적 고려가 빈약한 것이 이 모델의 가장 큰 약점으로 지적되어 왔다. 최근 미국 환경부는 EFDC(Environmental Fluid Dynamics Code) 라는 3차원 수리동역학 프로그램을 이용하여 대상 수체의 수리학적 거동을 모의하고 그 결과를 WASP7 에 연계시킬 수 있도록 하여 기존의 단점을 대폭 보완하였다. 본 연구에서는 금강 상류에 위치하고 있는 용담호를 대상으로 EFDC 를 이용하여 2005년 1년간 수위 및 수온성층현상을 예측하고 그 결과가 WASP 에 연결되어 사용될 수 있도록 하였다. 적절한 격자의 수를 결정하기 위하여 다양한 경우가 시행착오적으로 시험되었으며 비교적 적은 숫자의 격자로도 수위 및 수온의 모의가 가능하다는 것을 발견하였다.

• Transactions of the Korean Society of Mechanical Engineers B
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• v.34 no.8
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• pp.775-782
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• 2010

This study is performed to study the effect of the tray in the absorber of a flue-gas desulphurization (FGD) system by using a computational fluid dynamic (CFD) technique. Stagnant time of slurry and the pressure drop in the FGD absorber increase when a tray is used in the absorber. Stagnant time of slurry results in an increase in the desulfurization effect and a decrease in the power of the absorber recirculation pump; however, increased pressure drop requires more power of booster fan in the FGD system should be increased. The gas and slurry hydrodynamics inside the absorber is simulated using a commercial CFD code. The continuous gas phase has been modeled in an Eulerian framework, while the discrete liquid phase has been modeled by adopting a Lagrangian approach by tracking a large number of particles through the computational domain. It was observed that the power saved upon increasing the stagnant time of slurry was more than increased power with pressure drop.