이 연구에서는 안전관리체제(ISM Code) 실행지원 모듈개발중 하나인 ISM Code 운영평가 모듈 개발을 위한 기초적 연구를 수행하였다. 특히 ISM Code 운영평가 모듈 개발을 중심으로 AHP의 운영평가 분석과정과 설문지 설계, 운영평가 모형 기준의 위계 구조를 정립하였다는 것에 대해 그 의미가 있겠다. 또한 경영과학 분야의 주요 의사결정 하나인 AHP 기법을 운영평가 모듈 개발에 적용을 시도했다는 것에 대해서도 한층 가치가 있겠다.

It was general that WSD, USD, LSD etc. used in old do not consider area situation of each country and environment differences. But if concept of PBD which is supplement shortcoming of old design method and optimized design is introduced construction could be designed economical and plan systematically. It is purposed that this paper informs explanation and present condition for material and construction part of Asia Concrete Model Code. Also PBD design details which is suitable in comprehensive substance will be presented later.

이 논문은 해상보안체제의 도입방향을 연구하기 위한 것이다. 최근 2, 3년 사이에, 몇 편의 논문이 ISPS Code에 관한 연구를 다루고 있다. 2002년 12월 런던에서 개최된 해상보안에 관한 외교회의에서는 해상보안의 강화를 위하여 1974년 해상인명안전협약의 새로운 규정 및 본 보안규칙을 채택하였다. 이러한 새로운 요건들을 통하여 선박과 항만이 서로 협력하는 가운데 해상수송 분야의 보안을 위협하는 행위들을 감지하고 막을 있는 국제적인 체제가 형성되어질 수 있도록 하였다. 따라서 이 논문의 목적은 ISPS Code를 이해하고 해상보안체제의 도입방향을 제시하는 데 있다.

IMO는 1994년 해양안전 및 해양환경보호를 위해 ISM Code를 채택하였으며, 2002년 12월 선박, 선원, 화물, 항만시설의 안전을 도모하기 위해 ISPS Code를 채택하였다. ISPS Code는 2004년 1월부터 발효되는바, 해운회사 및 항만당국은 본 규정의 시행에 매우 촉박한 상태이다. ISM Code와 ISPS Code는 ISO 9001의 경영시스템 개념에 기초하고 있지만 목적은 다르다. 따라서 이들 세 기준들의 요건들을 비교분석하는 것은 매우 의미가 있을 것이다. 본 고에서는 이들 세 기준들의 배경, 원리, 요건들을 비교분석하고 해운계가 ISPS Code에 적합하게 보안조치를 수립하고 이행하는데 참고가 될 제안을 제시한다.

We investigate the morphology of Active Galactic Nuclei(AGN) jets. AGN jets propagate over kpc ~ Mpc and their beam velocities are close to the speed of light. The reason why many jets propagate over so long a distance and sustain a very collimated structure is not well understood. It is argued that some dimensionless parameters, the density and the pressure ratio of the jet beam and the ambient gas, the Mach number of the beam, and relative speed of the beam compared to the speed of light, are very useful to understand the morphology of jets namely, bow shocks, cocoons, nodes etc. The role of each parameters has been studied by numerical simulations. But more research is necessary to understand it systematically. We have developed 2D relativistic hydrodynamic code to analyze relativistic jets. We pay attention to the propagation velocity which is derived from 1D momentum balance in the frame of the working surface. We show some of our models and discuss the dependence of the morphology of jets on the parameter.

As a companion to an adiabatic version developed by Ryu and his coworkers, we have built an isothermal magnetohydrodynamic code for astrophysical flows. It is suited for the dynamical simulations of flows where cooling timescale is much shorter than dynamical timescale, as well as for turbulence and dynamo simulations in which detailed energetics are unimportant. Since a simple isothermal equation of state substitutes the energy conservation equation, the numerical schemes for isothermal flows are simpler (no contact discontinuity) than those for adiabatic flows and the resulting code is faster. Tests for shock tubes and Alfven wave decay have shown that our isothermal code has not only a good shock capturing ability, but also numerical dissipation smaller than its adiabatic analogue. As a real astrophysical application of the code, we have simulated the nonlinear three-dimensional evolution of the Parker instability. A factor of two enhancement in vertical column density has been achieved at most, and the main structures formed are sheet-like and aligned with the mean field direction. We conclude that the Parker instability alone is not a viable formation mechanism of the giant molecular clouds.

PMDSPH is a combined 3D particle-mesh and SPH code aimed to simulate the self-consistent dynamical evolution of spiral galaxies including live stellar and collisionless dark matter components, as well as an isothermal gas component. This paper describes some aspects of this code and shows how its application to the Milky Way helps to recover the gas flow within the Galactic bar region from the observed HI and CO longitude-velocity distributions.

This paper describes the numerical solution to the hyperbolic system of magnetohydrodynamic (MHD) equations. First, by pointing out the approximations involved, the deal MHD equations are presented. Next, the MHD waves as well as the associated shocks and discontinuities, are presented. Then, based on the hyperbolicity of the ideal MHD equations, the application of upwind schemes, which have been developed for hydrodynamics, is discussed to solve the equations numerically. As an definite example, one and multi-dimensional codes based on the Total Variation Diminishing scheme are presented. The treatment in the multi-dimensional code, which maintains ∇·B = 0, is described. Through tests, the robustness of the upwind schemes for MHDs is demonstrated.

SPH is the shorthand for Smoothed Particle Hydrodynamics. This method is a Lagrangian method which means that it involves following the motion of elements of fluid. These elements have the characteristics of particles and the method is called a particle method. A useful review of SPH (Monaghan 1992) gives the basic technique and how it can be applied to numerous problems relevant to astrophysics. You can get some basic SPH programs from http) /www.maths.monash.edu.au/jjm/sphlect In the present lecture I will assume that the student has studied this review and therefore understands the basic principles. In today's lecture I plan to approach the equations from a different perspective by using a variational principle.

본 연구에서는 지반상태가 교량의 지진응답에 미치는 영향을 분석하기 위해 다양한 지반모델 상의 교량모델에 대한 지진해석을 수행하고 그 결과를 비교.분석하였다 이를 위해서 기존의 교량시방서에서 분류된 네가지의 서로다른 지반종류를 대상으로 보다 세분된 지반모델 상에 위치하는 대표적인 교량에 대한 지진해석을 수행함으러써 첫째로는 각 지반 종류 상호간의 지진응답 차이의 정도를 시방서 값과 비교.분석하였으며 둘째로는 동일 지반으로 분류되는 상이한 두 지반간의 응답차이의 정도를 확인하였다 해석을 위해서는 시방서에서 제시된 두가지 방법 즉 단일모드 스펙트럼해석법과 다중모드 스펙트럼해석법을 사용하였으며 이들 결과를 별도로 작성된 인공시간이력을 입력으로 하는 시간이력해석법을 사용한 결과와 비교.분석하였다 시간이력해석법에서는 진동수에 무관한 지반임피던스함수를 이용하는 시간영역해석법을 사용하였다 해석결과 시방서에서 제시한 단일모드 및 다중모드 스펙트럼해석방법은 일반적으로 안전측의 지반-구조물 상호작용 해석결과를 주는 것으로 확인되었다 그러나 유연성이 큰 지반 상의 구조물에대한 지진해석을 위한 해석모델 작성시에는 지반의 유연성이 반드시 고려되어야 하며 특히 낙교방지를 위한 변위는 지반의 유연성을 고려한 정밀해석법에 의한 계산이 필수적으로 요구됨을 확인하였다.

We present a code which identifies individual clouds in crowded region using IMFORT interface within Image Reduction and Analysis Facility (IRAF). We define a cloud as an object composed of all pixels in longitude, latitude, and velocity that are simply connected and that lie above some threshold temperature. The code searches the whole pixels of the data cube in efficient way to isolate individual clouds. Along with identification of clouds it is designed to estimate their mean values of longitudes, latitudes, and velocities. In addition, a function of generating individual images (or cube data) of identified clouds is added up. We also present identified individual clouds using a 12CO survey data cube of Galactic Anticenter Region (Lee et al. 1997) as a test example. We used a threshold temperature of 5σ 5σ rms noise level of the data With a higher threshold temperature, we isolated subclouds of a huge cloud identified originally. As the most important parameter to identify clouds is the threshold value, its effect to the size and velocity dispersion is discussed rigorously.

현행 내진설계 규준에서 사용하고 있는 반응수정계수는 설계지진하중과 유사한 지진발생시 구조물이 비선형 거동을 하도록 탄성응답에서 요구되는 밑면전단력 값을 낮추는 계수라 할 수 있다. 따라서 반응수정계수는 하중저감계수(force reduction factor)라고 할 수 있으며, 이러한 값들은 경험적으로 결정된 것이어서 예상지진에 대하여 구조설계자가 설계한 건물이 어느정도의 비선형 거동을 할지는 예측하기가 힘들다. 본 연구에서는 목표가 되는 연성비(target ductility ratio)에 따라 요구되는 밑면전단력의 값을 구하고 이를 규준에서 요구하는 값과 비교할 것이다. 만약 요구되는 값이 규준 값 보다 크다면 이는 구조물이 가지는 부가강도(overstrength)나 잉여력(redundancy)이 담당해야 한다. 모멘트연성골조 건물을 설계한 후 이를 push-over 해석에 의하여 부가강도를 찾아 보아 요구강도와 비교할 것이다.

We have developed a cosmological N-body code which can simulate unprecedently large number of massive particles. This code is based on the Particle-Mesh scheme, and utilize the recent fast I/O devices to swap all variables. Using the new code we have simulated the formation and evolution of structures at high redshifts in the standard Cold Dark Matter (CDM) cosmogony. A simulation evolving 1024^3 particles on a 2048^3 mesh with the initial standard CDM power spectrum is being made. This is the first billion particle cosmological simulation with initial conditions representing the theoretical model over the widest range of space. A smaller, but still very large CDM simulation with 512^3 particles on a 1024^3 mesh has been completed. We have found that the galaxy-scale CDM halos with diameters of tens of kpcs undergo complete collapse before redshift 10. Our results clearly indicate that galactic and subgalactic structures have formed far before redshift 5 which is the present upper limit to the epoch of observed structures. We emphasize that the non-linear evolution of the galactic and subgalactic-scale structures starts as early as z ~ 50, and that cosmological simulations must start at such high redshifts. A high mass resolution is also indispensable to accurately represent the theoretical model in the initial conditions down to subgalactic scales, and to correctly study the subsequent formation and evolution of structures through hierarchical clustering.

The application of all regulations during building phase, plus constant vigilance in operation is essential to reducing the risk of fire aboard. A Safety by design approach is increasingly important. Fire safety regulation can solve problems which are hard to be solved by HSC code(International Code of Safety for High Speed Craft). Recently HSC code is applied for ship design development or guidance to the designer and demonstrates many advantages. In this pages, ship fire Safety are realistically modeled as ship design and the shipboard fires & muster stations are analyzed using HSC Code

We describe the implementation of a multi-dimensional numerical code to solve the equations for idea! magnetohydrodynamics (MHD) in cylindrical geometry. It is based on an explicit finite difference scheme on an Eulerian grid, called the Total Variation Diminishing (TVD) scheme, which is a second-order-accurate extension of the Roe-type upwind scheme. Multiple spatial dimensions are treated through a Strang-type operator splitting. Curvature and source terms are included in a way to insure the formal accuracy of the code to be second order. The constraint of a divergence-free magnetic field is enforced exactly by adding a correction, which involves solving a Poisson equation. The Fourier Analysis and Cyclic Reduction (FACR) method is employed to solve it. Results from a set of tests show that the code handles flows in cylindrical geometry successfully and resolves strong shocks within two to four computational cells. The advantages and limitations of the code are discussed.