Nonthermal particles can be produced due to incomplete thermalization at collisionless shocks and further accelerated to very high energies via diffusive shock acceleration. In a previous study we explored the cosmic ray (CR) acceleration at cosmic shocks through numerical simulations of CR modified, quasi-parallel shocks in 1D plane-parallel geometry with the physical parameters relevant for the shocks emerging in the large scale structure formation of the universe (Kang & Jones 2002). Specifically we considered pancake shocks driven by accretion flows with Uo = 1500 km s-l and the preshock gas temperature of To = 10 4 - 10 8K. In order to consider the CR acceleration at shocks with a broader range of physical properties, in this contribution we present additional simulations with accretion flows with Uo = 75 - 1500 km s-l and To = 10 4K. We also compare the new simulation results with those reported in the previous study. For a given Mach number, shocks with higher speeds accelerate CRs faster with a greater number of particles, since the acceleration time scale is tacc ∝ Uo-2. However, two shocks with a same Mach number but with different shock speeds evolve qualitatively similarly when the results are presented in terms of diffusion length and time scales. Therefore, the time asymptotic value for the fraction of shock kinetic energy transferred to CRs is mainly controlled by shock Mach number rather than shock speed. Although the CR acceleration efficiency depends weakly on a well-constrained injection parameter, є, and on shock speed for low shock Mach numbers, the dependence disappears for high shock Mach numbers. We present the 'CR energy ratio', Φ(Ms), for a wide range of shock parameters and for є = 0.2 - 0.3 at terminal time of our simulations. We suggest that these values can be considered as time-asymptotic values for the CR acceleration efficiency, since the time-dependent evolution of CR modified shocks has become approximately self-similar before the terminal time.

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.

In this study, vertical acceleration of center of mass was observed along normal gait phases in 9 healthy male volunteers (aged ). The developed wireless accelerometric device was attached on the intervertebral space between L3 and L4 using a semi-elastic waist belt. A three-dimensional motion analysis system, synchronized with the accelerometry, was used for detecting gait phases. There was no significant correlation between the body weight and the acceleration. The first peak curve covered loading response phase. The second downward peak point was matched accurately with the opposite toe-off. In mid-stance and terminal stance, the acceleration curve highly resembled the vertical ground reaction force curve. There was no significant difference in timing between the final upward peak point and the initial contact. Therefore, the developed accelerometry system would be helpful in determining determine temporal gait pattems in patients with gait disorders.

A numerical scheme that incorporates a self-consistent cosmic-ray (CR, hereafter) injection model into the combined gas dynamics and CR diffusion-convection code has been developed. The hydro/CR code can follow in a very cos-effective way the evolution of CR modified shocks by adopting subzone shock-tracking and multi-level Adaptive Mesh Refinement techniques. The injection model is based on interactions of the suprathermal particles with self-generated MHD waves in quasi-parallel shocks. The particle injection is followed numerically by filtering the diffusive flux of suprathermal particles across the shock to upstream region according to a velocity-dependent transparency function, which represents the fraction of leaking suprathermal particles. In the strong shock limit of Mach numbers ≥ 20, significant physical processes such as the injection and acceleration seem to become independent of M, while they are sensitively dependent on M for M < 10. Although some particles injected early in the evolution continue to be accelerated to higher energies, the postshock CR pressure reaches a time asymptotic value due to balance between acceleration and diffusion of the CR particles.

To study the structure and dynamics of a cosmic-ray-plasma system, hydrodynamic approach is a fairly good approximation. In this approach, there are three basic energy transfer mechanisms: work done by the plasma flow against pressure gradients, cosmic ray streaming instability and stochastic acceleration. The interplay between these mechanisms gives a range of structures. We present some results of different version of the hydrodynamic approach, e.g., flow structure, injection, instability, acceleration with and without shocks.

Cosmic-ray acceleration, although physically important in many astrophysical contexts, is difficult to incorporate into numerical models,. because it involves microphysics that is generally far from thermodynamic equilibrium, and also because the length and time scales for that physics typically range over many orders of magnitude, reflecting the huge range of particle rigidities that must be represented. The most common accelerator models are stochastic in nature and involve nonequilibrium plasma properties that are also often poorly understood. Still, nature clearly finds a way to produce simple, robust and almost scale-free energy distributions for the cosmic-rays. Their importance has inspired a number of approaches to examining the production and transport of cosmic-ray particles in numerical simulations. I offer here a brief comparison of some of the methods that have been introduced.

Rarefied cosmic plasmas generally do not achieve thermodynamic equilibria, and a natural consequence of this is the presence of a significant population of charged particles with energies well above those of the bulk population. These are exemplified by the galactic cosmic rays, but the importance of these high energy populations extends well beyond that context. I review here some of the basic issues associated with the propagation and acceleration of cosmic rays, especially in the context of collisionless plasma shocks.

지진가속도에 의한 부재의 지진거동 특성은 실험적인 방법 또는 등가의 정적실험으로부터 추정되어 온 것이 대부분이다 본 연구에서는 지진가속도에 의한 철근콘크리트 전단벽체의 지진응답 및 파괴거동 특성을 유한요소법을 사용한 해석적인 기법에 의해서 예측하였다 콘크리트 부재에서 균열은 필연적으로 발생하게 되며 이로 인한 부재의 강도 및 강성의 감소 철근의 항복 및 하중의 반복성으로 인한 균열의 개폐등이 수반된다 본 연구에서는 이와 같은 콘크리트와 철근의 비선형 특성을 고려한 이축응력상태에 대한 재료모델과 동적해석 알고리즘을 범용 수치해석기법인 유한요소법을 사용하여 해석프로그램으로 구현하였다 지진가속도를 받는 전단벽을 대상으로 지진응답 및 파괴거동등을 본 연구의 해석적인 방법으로 예측하였으며 그 결과를 신뢰성 있는 연구자의 실험결과와 비교하여 그 타당성을 검증하였다.

대형 시스템의 건전성 평가를 위한 동적 재하시험에 있어서 변위를 측정하는 것보다 가속도를 측정하는 것이 수월하나 대부분의 공학적 기준은 응력과 비례관계를 지니는 변화를 기준으로 하고 있다. 본 연구에서는 시스템의 재하시험시 측정된 가속도신호를 이용하여 변위응답을 산정하는데 그 목적을 두고 적분을 위한 신호처리시 발생되는 문제점을 정상상태 및 천이영역에 대하여 규명하였다. 기존의 연구에서 고려하지 못하였던 초기조건의 항을 도입함으로써 시간영역의 적분과 주파수영역의 적분결과가 일치함을 해석적으로 입증하였으며 이동하중을 받는 보의 동적거동에 대하여 제시된 타당성을 검증하였다.

최근의 중.소규모의 연이은 지진활동은 한반도도 지진에 대하여 안전지대는 아닌 것으로 생각되고 있으며, 1995년 일본의 Kobe 지진 대 참사는 국내에도 지진에 관한 많은 관심을 고조시키고 있다. 그러나, 국내의 구조물의 내진설계를 위한 사용되는 지진파에 대한 연구는 매우 미흡하며, 최근까지도 국내에서는 외국의 설계용 지진파를 그대로 사용하거나 설계응답스펙트럼을 이용하고 있는 실정이다. 본 논문에서는 국내지진파의 물리적 특성, 즉, 주기-빈도 분포, 확률밀도분포, Fourier Spectrum 및 응답스펙트럼을 구하여 비교.분석하였다. 또한 이상화된 인공지진파를 산출하여 이를 현재 교통량의 폭발적인 증가와 도로의 선형성을 이유로 사각을 가진 교량구조물이 많이 건설되고 있는바, 70^{\circ}사각슬래브교에 대한 지진해석을 수행하여 인공지진의 합리적 해석 횟수를 규명하였다.

변위응답은 교량구조의 진동특성을 결정하는데 중요한 인자 중의 하나이다. 계측된 가속도 데이타를 진동수 영역에서 적분하여 변위응답을 경제적이고 합리적으로 구할 수 있다. 이를 위해 계측된 가속도 데이타를 이산화하기 위해 적절한 표본추출 진동수가 제시되었다. 캔틸레버 보를 이용한 실내시험에서 직접 계측된 변위와 적분된 변위는 서로 잘 일치하였다. 평가된 변위응답으로부터 구한 모우드 형상도 해석치와 근접하므로 개발된 방법은 실제로 효율적으로 사용될 수 있음을 입증하였다.

In order to explore the time dependence of the closure parameters of the two-fluid calculations for supernova remnants and the terminal shocks of stellar winds, we have considered a simple model in which the time evolution of the cosmic-ray distribution function was followed in the test-particle limit using the Bohm diffusion model. The particles are mostly accelerated to relativistic energy either in the free expansion phase of the SNRs or in the early phase of the stellar winds, so the evolution of the closure parameters during these early stages is substantial and should be followed correctly. We have also calculated the maximum momentum which is limited by either the age or the curvature of these spherical shocks. We found that SNRs expanding into the medium where the gas density decreases with the distance from the explosion center might be necessary to explain the observed power-law distribution of the galactic cosmic rays. The energy loss due to the escaping energetic particles has been estimated for the terminal shocks of the stellar winds.

By comparison and analysis of the optical data of the two galactic clusters of Pleiades and h and x Persei and the radio data of the HI gas clouds which are related with those two clusters, the relative motions of those gas clouds with retpect to the two clusters were obtained. The three theories on the acceleration of HI gas cloud surrounding a star cluster by Blaauw. Oort and Spitzer, and Kahn were examined with the above obtained kinetic data of the Pleiades and the h and x Penei clouds. And it was shown that Blaauw's theory is applicable to the h and x Persoi clouds but not to the Pleiades, that Dart and Spitzer's theory can explain the motions of both clouds, and that Kahn's theory needs more improvement to be a complete one.

본 연구는 길이 1m의 SD400 D13, D10 철근 시편의 중앙 20cm를에 염화칼슘(CaCl2–10%)과 10V의 전압을 인가하여 부식을 촉진시킨 수, 부식으로 인해 줄어든 단면적과 철근의 인장 거동과의 관계를 파악하기 위한 것이다. 9주 동안의 실험을 통해 평균 15.57%의 단면 손실을 이루었으며, 이때 부식이 진행된 시편에서 항복응력의 저하, 탄성계수 감소 등의 현상이 나타난 것을 확인할 수 있다.

1990년대 초반 다양한 시설물 붕괴사고와 인해 발생하는 국가적인 재산손실과 국민의 안전성 확보를 위한 시설물안전관리 특별법이 재정되었으나 최근 건축 및 토목 구조물 등 30년 이상의 노후 된 시설물의 급속한 증가 및 인건비증가, 공기단축, 민원증가로 P.C구조물의 공사가 증가됨에 따라 P.C구조물을 포함한 안전점검 및 유지관리를 위한 정밀안전진단의 필요도와 중요도는 높아졌으나 수행 기술자의 기술 숙련도에 따라 진단결과와 측정 정밀도에 영향을 미치므로 본 연구에서는 P.C구조물의 안전진단을 위한 3축(X, Y, Z축) 가속도 측정 센서 부착 시 P.C구조물의 구조해석을 통한 모드분석을 수행하여 센서 의 최적 위치 도출에 대한 연구가 필요한 실정이다.

현재 이루어지는 구조물의 안전진단과 성능에 대한 정밀검사는 기술자에 의해 수행되어 측정된 데이터가 경험적 판단에 의해 변화될 수 있는 수준에 머물러 있는 실정으로 본 연구에서는 프리캐스트 콘크리트 구조물을 실제 현장에서 이루어지는 설치방법과 동일하게 설치 후 기존 동적센서와 3축(3측(X, Y, Z축) 가속도 측정 센서 부착하여 손상정도에 따른 가속도 응답과 FFT분석 결과를 비교하여 P.C구조물의 안전진단에 대한 데이터의 불확실성에 대한 개선과 교체시기, 손상예측 등에 대한 기초자료로 활용하기 위함이다.

Currently, the cable safety management of cable supported bridges is calculated by the ratio of the measured tension to the design tension. The measurement of the tension is performed by indirectly estimating the acceleration measured at the cable surface in terms of the tension. The method of converting the cable vibration response (acceleration) into the tension is disadvantageous in that the damage of the individual strand (or wire) in the cable is not clearly reflected in the tension because the measurement is not reliable and is managed only by the total tension. The purpose of this study is to improve the cable safety management system by evaluating how the damage of individual strand of MS type cable, which is mainly applied to cable-stayed bridges, affects the safety level managed by level of cable tension.