• 한국자동차공학회논문집
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• 제9권4호
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• pp.50-55
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• 2001

To simulate the combustion process under stratified charged conditions, like GDI engines, the new combustion model is proposed, which is based on Welter's FAE model and Peters' PDF model for considering primary reactions. In addition to these models, the new laminar burning velocity correlation and diffusion flame model are also included in the proposed model. The former can be applicable to much wider range of equivalence ratio, pressure and temperature than the others, such as Keck's and Guilder's models, and the latter has been derived from water-gas shift reaction and hydrogen oxidation, by which the secondary reactions can be considered after primary reactions. 3-D computation has been performed by using STAR-CD v3.05 in the simple cylindrical geometry under stratified charged condition. Judging from the calculated results, the present model proves to be reasonable to simulate the characteristics of flame propagation and concentrations of products in burned regions.

• 천문학회보
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• 제36권1호
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• pp.56.1-56.1
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• 2011

To understand the effect of the initial rotation for tidally bounded clusters with mass spectrum, we performed N-body simulations for the clusters with different degrees of initial rotation and compared to Fokker-Planck results. We confirmed that the cluster evolution is accelerated by the initial rotation as well as the mass spectrum. For the slowly rotating models, the time evolution of mass, energy and angular momentum show good agreements between N-body and Fokker-Planck calculations. On the other hand, for the rapidly rotating models, there are significant differences between two approaches at the beginning of the evolution. By investigating cluster shapes, we concluded that these differences are mainly due to secular instability that takes place for very rapidly rotating clusters. The shape of cluster for N-body simulations becomes tri-axial or even prolate, while the 2-dimensional Fokker-Planck simulation can treat only oblate type axisymmetric systems. We also founded that there is the angular momentum exchange from high mass to low mass.

• 천문학회보
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• 제36권1호
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• pp.84.2-84.2
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• 2011

Astrophysical jets play important roles in many interesting astronomical phenomena, such as star formation, gamma-ray bursts, and active galactic nuclei. The jets are thought to be driven by rotating disks through magneto-centrifugal processes. However, quantitative understanding of the jet-driving mechanism has been difficult because examples showing rotation in both disk and jet are rare. One of the important quantities in the models of jet engine is the size of the jet-launching region. The bipolar jet of the NGC 1333 IRAS 4A2 protostar shows a lateral velocity gradient, which suggests that the SiO jet is rotating around its axis. The jet rotation is consistent with the rotation of the accretion disk. The disk-jet rotation kinematics suggests that the jet-launching region on the disk, or the outflow foot-ring, has a radius of about 2 AU, which supports the disk-wind models.

• 한국정보처리학회:학술대회논문집
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• 한국정보처리학회 2012년도 추계학술발표대회
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• pp.1555-1558
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• 2012

제품 라인 공학의 핵심은 여러 제품 개발에 쉽게 재사용 될 수 있는 핵심 자산의 개발과 산출된 핵심자산을 이용하여 원하는 제품을 생산함에 있다. 그렇기 때문에 제품 라인 공학에서 원하는 제품 모델을 적기에 생산해내도록 도와주기 위하여, 제품 라인 모델의 자산으로부터 제품 모델을 추출해주는 도구를 필요로하게 된다. 사용자가 필요로하는 제품 라인 산출물의 추출을 도와주기 위해서는 제품 라인 모델로 산출될 수 있는 모든 모델을 고려할 필요가 있다. 하지만 모든 제품 라인 모델로부터 제품 모델을 추출하는 모듈을 개별적으로 구현하는 것은 비생산적이다. 따라서 본 연구에서는 사용자 맞춤형 제품 모델 추출 도구의 구현을 위해, 오픈 소스인 StarUML을 이용하여 제품 모델 추출 기법의 일반화를 제안한다.

• 한국공간구조학회논문집
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• 제12권1호
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• pp.59-68
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• 2012

대공간 구조시스템의 하나인 스페이스 프레임 구조는 종횡의 부재가 3차원적으로 연결되어 입체적으로 외부 힘에 저항하는 구조로써 높은 강성을 갖는다. 또한 균등한 응력 분담이 가능하도록 설계되는 스페이스 프레임 고유의 역학적 특성에 기인하여 경량화가 가능하다. 스페이스 프레임의 구조안정 문제는 구조물의 여러 가지 조건에 따라 결정되며 매우 중요하다. 본 연구에서는 기하학적 형태에 따른 래티스 돔의 동적구조불안정 특성을 알아보기 위해 2-자유 절점 구조물을 통해 스페이스 프레임의 붕괴 메터니즘을 파악하고, 기하학적 형태에 따라 Star Dome, Parallel Lamella Dome, 3-Way Grid Dome을 모델로 선택하여 동일레벨의 주기성이 없는 STEP 하중에 의한 동적외력 하에서의 라이즈-스팬(${\mu}$)비 및 형상불완전에 따른 불안정 거동 특성을 알아본다.

• 한국공간구조학회논문집
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• 제12권2호
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• pp.109-118
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• 2012

주기성을 가진 하중하에서의 거동은 스텝하중하에서의 거동과는 다른 거동을 보일 것이라 예상된다. 본 연구에서는 기하학적 형태에 따른 래티스 돔 구조물을 정현파 하중에서의 동적구조불안정 특성을 알아본다. 대공간 구조시스템의 하나인 스페이스 프레임 구조는 종횡의 부재가 3차원적으로 연결되어 입체적으로 외부 힘에 저항하는 구조로써 높은 강성을 갖는다. 또한 균등한 응력 분담이 가능하도록 설계되는 스페이스 프레임 고유의 역학적 특성에 기인하여 경량화가 가능하다. 스페이스 프레임의 구조안정문제는 구조물의 여러 가지 조건에 따라 결정되고 매우 중요한 사항이다. 따라서 기하학적 형태에 따라 Star Dome, Parallel Lamella Dome, 3-Way Grid Dome을 모델로 선택하여 라이즈-스팬(${\mu}$)비 및 형상불완전에 따른 불안정 거동 특성을 알아본다. 전체적으로 래티스 돔 구조물은 비감쇠 보다 감쇠를 도입한 경우 동적 좌굴하중에 대한 효율이 높아짐을 알 수 있다.

• 천문학회보
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• 제37권2호
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• pp.73.2-73.2
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• 2012

Matusoka & Kawara (2010) showed that the number density of the most massive galaxies (log $M/M_{\odot}=11.5-12.0$) increases faster than that of the next massive group (log $M/M_{\odot}=11.0-11.5$) during 0 < z < 1. This appears to be in contradiction to another important empirical concept of "downsizing". We attempt to understand the two observational findings in the context of the hierarchical merger paradigm using semi-analytic techniques. Our models closely reproduce the result of Matusoka & Kawara (2010). Downsizing can also be understood as larger galaxies have on average smaller assembly ages but larger stellar ages. Our fiducial models further reveal the details on the history of stellar mass growth of massive galaxies. The most massive galaxies (log $M/M_{\odot}=11.5-12.0$ at z=0), which are mostly brightest cluster galaxies, obtain roughly 70% of their stellar components via merger accretion. The role of merger accretion monotonically declines with galaxy mass: 45% for log $M/M_{\odot}=11.0-11.5$ and 20% for log $M/M_{\odot}=10.5-11.0$ at z = 0. The specific accreted stellar mass rates via galaxy mergers decline very slowly during the whole redshift range, while the specific star formation rates sharply decrease with time. In the case of the most massive galaxies, merger accretion becomes the most important channel for the stellar mass growth at z ~ 2. On the other hand, in-situ star formation is always the dominant channel in the $L_*$ galaxies.

• Nuclear Engineering and Technology
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• 제42권6호
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• pp.656-661
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• 2010

Lead-alloys are very attractive nuclear coolants due to their thermo-hydraulic, chemical, and neutronic properties. By utilizing the HELIOS (Heavy Eutectic liquid metal Loop for Integral test of Operability and Safety of PEACER$^2$) facility, a thermal hydraulic benchmarking study has been conducted for the prediction of pressure loss in lead-alloy cooled advanced nuclear energy systems (LACANES). The loop has several complex components that cannot be readily characterized with available pressure loss correlations. Among these components is the core, composed of a vessel, a barrel, heaters separated by complex spacers, and the plenum. Due to the complex shape of the core, its pressure loss is comparable to that of the rest of the loop. Detailed CFD simulations employing different CFD codes are used to determine the pressure loss, and it is found that the spacers contribute to nearly 90 percent of the total pressure loss. In the system codes, spacers are usually accounted for; however, due to the lack of correlations for the exact spacer geometry, the accuracy of models relies strongly on assumptions used for modeling spacers. CFD can be used to determine an appropriate correlation. However, application of CFD also requires careful choice of turbulence models and numerical meshes, which are selected based on extensive experience with liquid metal flow simulations for the KALLA lab. In this paper consistent results of CFX and Star-CD are obtained and compared to measured data. Measured data of the pressure loss of the core are obtained with a differential pressure transducer located between the core inlet and outlet at a flow rate of 13.57kg/s.

• BMB Reports
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• 제40권1호
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• pp.119-124
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• 2007

Adenoviral vectors are among the most promising vectors available for human gene therapy. However, the use of recombinant adenoviral vectors, including replicationcompetent adenovirus (RCA), raises a variety of safety concerns in relation to the development of new therapies based on gene therapy. To examine how organic compounds change in rat plasma following the injection of adenovirus, $\beta$-galactosidase expressing recombinant adenovirus (designated rAdLacZ) or RCA, we investigated the content of fatty acids (FAs), which are important biochemical indicators in pathological conditions. Pattern recognition analysis on the level of FAs in rat plasma is described for the visual discrimination of adenovirus infection groups from normal controls. Plasma FAs from four control rats (normal group), and from four rats with rAdLacZ infection and six rats with RCA infection (the two abnormal groups), were examined by gas chromatography-mass spectrometry in selected ion monitoring modes as their tert-butyldimethylsilyl derivatives. In total, 20 FAs were positively detected and quantified. The results of the Student's t-test on the normal mean of two abnormal groups, the levels of three FAs (p<0.05) from rAdLacZ group and eleven FAs (p<0.05) from RCA group were significantly different. When star symbol plotting was applied to the group mean values of 20 FAs after normalization to the corresponding normal mean values, the resulting eicosagonal star patterns of the two infected groups were distorted into similar shapes, but were distinguishable from each other. Thus, these approaches will be useful for screening and monitoring of diagnostic markers for the effects of infection following the use of adenoviral vectors in gene therapy.

• 천문학회지
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• 제36권3호
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• pp.167-175
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• 2003

There is accumulating evidence for a strong link between nuclear starbursts and AGN. Molecular gas in the central regions of galaxies plays a critical role in fueling nuclear starburst activity and feeding central AGN. The dense molecular ISM is accreted to the nuclear regions by stellar bars and galactic interactions. Here we describe recent observational results for the OB star forming regions in M51 and the nuclear star burst in Arp 220 - both of which have approximately the same rate of star formation per unit mass of ISM. We suggest that the maximum efficiency for forming young stars is an Eddington-like limit imposed by the radiation pressure of newly formed stars acting on the interstellar dust. This limit corresponds to approximately 500 $L_{\bigodot} / M_{\bigodot}$ for optically thick regions in which the radiation has been degraded to the NIR. Interestingly, we note that some of the same considerations can be important in AGN where the source of fuel is provided by stellar evolution mass-loss or ISM accretion. Most of the stellar mass-loss occurs from evolving red giant stars and whether their mass-loss can be accreted to a central AGN or not depends on the radiative opacity of the mass-loss material. The latter depends on whether the dust survives or is sublimated (due to radiative heating). This, in turn, is determined by the AGN luminosity and the distance of the mass-loss stars from the AGN. Several AGN phenomena such as the broad emission and absorption lines may arise in this stellar mass-loss material. The same radiation pressure limit to the accretion may arise if the AGN fuel is from the ISM since the ISM dust-to-gas ratio is the same as that of stellar mass-loss.