• 천문학회보
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• 제36권2호
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• pp.52.1-52.1
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• 2011

We have implemented the Smoothed Particle Hydrodynamics (SPH) into the cosmological N-body simulation code. The pre-initial particle distribution is set to follow the glacial conditions and the initial temperature of hydro particles is calculated based on the adiabatic process in the expanding backgrounds. Typical adiabatic SPH equations are adopted and, additionally, non-adiabatic processes such as heating/cooling and supernova explosion are added. We study the effect of star formation criteria on the global star formation rate and compare it with the observations.

• 한국해안·해양공학회논문집
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• 제23권3호
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• pp.193-204
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• 2011

역동적인 파랑에 노출되는 경우 다양한 failure mode를 쉽게 드러내는 Oil boom의 성능을 개선하기 위해 가장 정교한 파랑모형인 spatially filtered Navier-Stokes 식을 LES (Large Eddy Simulation), 잔차응력에 대한 LDS (Lagrangian Dynamic Smagorinsky 모형), SPH (Smoothed Particle Hydrodynamics) 기법을 활용하여 해석하는 새로운 수치모형이 제언되었다. 이어 부유식 Oil Boom의 누유특성을 규명하기 위해 oil spill, progressive wave, oil boom의 상호작용을 oil boom이 계류삭에 고정되어있는 경우와 oil boom의 excursion이 허용된 경우에 대해 각각 수치모의 하였다. 모의결과 oil boom의 skirt 길이가 수심의 30% 이상이고 excursion이 허용된 경우 oil spill의 차폐 기능은 극대화되는 것으로 밝혀졌다. 이와 더불어 y = 1~2 m 사이에 오일막과 해수의 경계층에서 생성된 와류가 저면으로 확산되면서 시계방향과 반 시계방향의 와류가 엇갈리게 생성되는 coherent eddies가 관측되어 수리실험을 통해 그 존재가 알려진 Kelvin-Helmholz파의 성장과정과 계면으로부터의 일탈과정이 수치모의된 것으로 판단된다.

• 한국식품과학회지
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• 제49권4호
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• pp.438-443
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• 2017

다양한 영양성분을 함유할 뿐만 아니라 생리활성이 우수한 참죽의 기능성 식품소재로의 이용가능성을 확인하고자 참죽으로부터 폴리페놀을 추출하고 이들의 생리기능성을 측정하였다. 이를 위해 동결건조된 참죽분말을 열수, 에탄올 및 효소(Viscozyme, Shearzyme)를 이용하여 폴리페놀을 추출하고 추출방법에 따른 폴리페놀 분획의 기능적 특성을 비교하였다. 참죽으로부터 추출된 폴리페놀 분획의 수율은 VphF가 43.44%로 가장 높았으며, 그 다음 SphF, WphF, EphF 순으로 나타났다. 총 폴리페놀 및 총 플라보노이드 함량은 EphF가 각각 447.98 mg GAE/g 및 337.49 mg QE/g으로 가장 높은 함량을 보였다. 산화방지 활성을 측정한 결과, DPPH 라디칼 소거능, ABTS 라디칼 소거능, $Fe^{2+}$ 킬레이팅 효과 및 환원력 모두 EphF가 유의적으로 가장 높았다. Acetylcholinesterase 저해활성을 측정한 결과, 저농도에서는 EphF가, 고농도에서는 WphF가 가장 높은 활성을 보였다. ${\alpha}$-glucosidase 저해활성은 EphF, VphF, SphF, WphF 순으로 높은 활성을 보였으며, 특히 EphF, SphF, VphF는 대조군인 아카보스보다 유의적으로 높은 활성을 보였다. Tyrosinase 저해활성 측정 결과, 2 mg/mL 농도에서 모든 추출군은 50% 이상의 저해활성을 보였다. 이상의 연구 결과, 참죽의 폴리페놀 분획은 우수한 산화방지 활성뿐만 아니라 ${\alpha}$-glucosidase, acetylcholinesterase, tyrosinase 효소에 대한 높은 저해활성을 보였으며, 특히 에탄올추출 및 열수추출에 의해 얻어진 폴리페놀 분획은 뛰어난 산화방지 활성을 보였다. 이를 통해 참죽은 기능성 식품 소재로 활용가능성이 매우 높을 것으로 판단된다.

• 천문학회지
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• 제34권4호
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• pp.313-315
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• 2001

Some authors have concluded that spiral structures and shocks do not develop if an adiabatic index $\gamma$ > 1.16 is adopted in accretion disc modelling, whilst others have claimed that they obtained well defined spirals and shocks adopting a $\gamma$ = 1.2 and a $M_2/ M_1$ = 1 stellar mass ratio. In our opinion, it should be possible to develop spiral structures for low compressibility gas accretion discs if the primary component is a black hole. We considered a primary black hole of 8M0 and a small secondary component of 0.5M$\bigodot$ to favour spiral structures formations and possible spiral shocks via gas compression due to a strong gravitational attraction. We performed two 3D SPH simulations and two 2D SPH simulations and characterized a low compressibility model and a high compressibility model for each couple of simulations. 2D models reveal spiral structures existence. Moreover, spiral shocks are also evident in high compressibility 2D model at the outer disc edge. We believe that we could develop even well defined spiral shocks considering a more massive primary component.

• 천문학회지
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• 제29권1호
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• pp.19-30
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• 1996

We have examined consequences of strong tidal encounters between a neutron star and a normal star using SPH as a possible formation mechanism of isolated recycled pulsars in globular clusters. We have made a number of SPH simulations for close encounters between a main-sequence star of mass ranging from 0.2 to 0.7 $M_\bigodot$ represented by an n=3/2 poly trope and a neutron star represented by a point mass. The outcomes of the first encounters are found to be dependent only on the dimensionless parameter $\eta'{\equiv}(m/(m+ M))^{1/2}(\gamma_{min}/R_{MS})^{3/2}(m/M)^{{1/6)}$, where m and M are the mass of the main-sequence star and the neutron star, respectively, $\gamma_{min}$ the minimum separation between two stars, and $R_{MS}$ the size of the main-sequence star. The material from the (at least partially) disrupted star forms a disk around the neutron star. If all material in the disk is to be acctreted onto the neutron star's surface, the mass of the disk is enough to spin up the neutron star to spin period of 1 ms.

• Nuclear Engineering and Technology
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• 제53권11호
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• pp.3543-3562
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• 2021

The methods and performance of a 3D pin-by-pin neutronics code based on the 2D/1D decoupling method are presented. The code was newly developed as an effort to achieve enhanced accuracy and high calculation performance that are sufficient for the use in practical nuclear design analyses. From the 3D diffusion-based finite difference method (FDM) formulation, decoupled planar formulations are established by treating pre-determined axial leakage as a source term. The decoupled axial problems are formulated with the radial leakage source term. To accelerate the pin-by-pin calculation, the two-level coarse mesh finite difference (CMFD) formulation, which consists of the multigroup node-wise CMFD and the two-group assembly-wise CMFD is implemented. To enhance the accuracy, both the discontinuity factor method and the super-homogenization (SPH) factor method are examined for pin-wise cross-section homogenization. The parallelization is achieved with the OpenMP package. The accuracy and performance of the pin-by-pin calculations are assessed with the VERA and APR1400 benchmark problems. It is demonstrated that pin-by-pin 2D/1D alternating calculations within the two-level 3D CMFD framework yield accurate solutions in about 30 s for the typical commercial core problems, on a parallel platform employing 32 threads.

• 대한토목학회논문집
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• 제28권5B호
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• pp.547-558
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• 2008

최근 폭증하는 해상물동량으로 인해 선박은 날로 대형화되며 현재 우리나라에서는 이러한 추이에 대응하기 위해 초대형 항만건설이 서둘러 진행되고 있으며 그 중 일부는 이미 부분적으로 완성되어 운영 중이거나 계속적인 확장이 예정되어있다. 초대형 항만의 경우 항 정온도 확보를 위해 대형 직립형 방파제가 수반되기 마련이나 비교적 높은 반사율로 인해 장주기의 파랑에 취약한 구조적 문제를 지닌다. 장주기 파랑의 효과적 제어를 위해 본 고에서는 아치형 curtain wall과 유수실로 구성된 된 장파 제어체 -Eco-breaker 2- 가 제시되며 Eco-breaker 2의 수리특성을 수치적으로 규명하였다. 수치모형은 가장 강건한 파랑모형인 Navier-Stokes Eq.과 SPH(Smoothed Particle Hydrodynamics), LES(Large Eddy Simulation) 기법에 기초하여 구성하였다. 수치모형의 검증을 위한 수리모형실험도 병행하였다. 수치모의 결과 Eco-breaker 2는 유수실 내부에 생성되어 아치형 curtain wall 전면 수역과 유수실을 주기적으로 넘나드는 대규모 구조적 와로 장파를 효과적으로 제어할 수 있었다. 또한 대규모 구조적 와의 생성 영역과 세기는 내습하는 파랑의 주기에 종속하며 유수실 체류시간이 입사파 주기의 반을 하회하는 경우 반사계수는 최대 0.18까지 낮아진다. 이러한 결과는 Eco-breaker 2가 환경친화적 항의 개발에 적극적으로 활용될 수 있음을 시사하는 것으로 이를 위해 그 구체적 제원도 함께 제시하였다.

• International Journal of Naval Architecture and Ocean Engineering
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• 제10권3호
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• pp.329-347
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• 2018

The Smoothed Particle Hydrodynamics (SPH) method has proved to have great potentials in dealing with the wave-structure interactions. Compared with the Weakly Compressible SPH (WCSPH) method, the ISPH approach solves the pressure by using the pressure Poisson equation rather than the equation of state. This could provide a more stable and accurate pressure field that is important in the study of wave-structure interactions. This paper improves the solid boundary treatment of ISPH by using a high accuracy Simplified Finite Difference Interpolation (SFDI) scheme for the 2D wave-structure coupling problems, especially for free-moving structure. The proposed method is referred as the ISPH_BS. The model improvement is demonstrated by the documented benchmark tests and laboratory experiment covering various wave-structure interaction applications.

• 천문학회보
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• 제43권2호
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• pp.54.3-55
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• 2018

We present the physical and environmental properties of nearby dwarf elliptical-like galaxies. The present sample consists of ~ 1,100 dwarf elliptical-like galaxies within redshifts 0.01. The morphological types of the present study were determined by Ann, Seo, and Ha (2015) who classified the dwarf elliptical-like galaxies by the five subtypes of dS0, dE, dSph, dEbc, and dEblue. We examine their star formation history using STARLIGHT. The star formation history of dwarf elliptical-like galaxies depends on their subtypes. The luminosities of dS0, dE, and dSph galaxies are dominated by the extremely old stars (${\geq}10^{10}yr$) with $z{\approx}0.0004$ while those of dEbc and dEblue galaxies are mainly due to the young (${\sim}10^7yr$) stars together with the nearly equal contribution by extremely young stars (${\sim}10^6yr$) and old (${\sim}10^9yr$) stars. Young populations have a variety of metallicity, from z=0.0001 to z = 0.04, while old populations have metallicity of z = 0.0001 and z = 0.0004. While the formation history of stars older than ~1010yr depends mainly on the luminosity of galaxies, the formation history of stars younger than ~108yr is mainly affected by their environment. However, luminosity and environment are equally important for the star formation history if there is no star formation at the early phase of galaxy formation.

• 천문학회보
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• 제36권2호
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• pp.58.2-58.2
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• 2011

We present smoothed particle hydrodynamic models of the interactions in the compact galaxy group, Stephan's Quintet. Adding thermohydrodynamic effects to the earlier collisionless N-body simulations of Renaud et al. (2010), we further investigate the dynamical interaction history and evolution of the intergalactic gas of Stephan's Quintet. Specifically, we model the formation of the hot X-ray gas, the group-wide shock, and emission line gas as the result of NGC 7318b colliding with the group as well as reproduce the tidal structures in the group. We compare our model results to multi-wavelength observations.