• 한국방사성폐기물학회:학술대회논문집
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• 한국방사성폐기물학회 2017년도 춘계학술논문요약집
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• pp.211-212
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• 2017

• 한국통신학회논문지
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• 제38A권12호
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• pp.1045-1053
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• 2013

본 논문에서는 Long-Term Evolution (LTE) 시스템에서 사용자 단말과 통신하는 상대노드 사이에 발생하는 양방향 지연을 고려하여 새로운 전력절감 알고리즘을 제안한다. 제안하는 전력절감 알고리즘은 양방향 지연을 겪는 트래픽 발생 패턴에 맞추어 기존 LTE 시스템의 전력절감 알고리즘에서 사용하는 단말 상태 천이 순서를 반대로 적용한다. 발생하는 양방향 지연을 수학적으로 모델링한 후 제안 전력절감 방식의 성능을 단말의 에너지 소비량과 패킷의 버퍼링 지연 관점에서 분석한다. 운용 파라미터의 변화에 따라 이들 성능을 에너지-지연 트레이드오프 곡선으로 특성화하고 이를 통해 제안하는 전력절감 방식이 기존 LTE 표준의 전력절감 방식과 비교하여 에너지와 지연 성능 모두를 효과적으로 향상시키고 있음을 확인한다.

• Nuclear Engineering and Technology
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• 제41권1호
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• pp.11-20
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• 2009

Radiation effects on materials are inherently multiscale phenomena in view of the fact that various processes spanning a broad range of time and length scales are involved. A multiscale modeling approach to embrittlement of pressure vessel steels is presented here. The approach includes an investigation of the mechanisms of defect accumulation, microstructure evolution and the corresponding effects on mechanical properties. An understanding of these phenomena is required to predict the behavior of structural materials under irradiation. We used molecular dynamics (MD) simulations at an atomic scale to study the evolution of high-energy displacement cascade reactions. The MD simulations yield quantitative information on primary damage. Using a database of displacement cascades generated by the MD simulations, we can estimate the accumulation of defects over diffusional length and time scales by applying kinetic Monte Carlo simulations. The evolution of the local microstructure under irradiation is responsible for changes in the physical and mechanical properties of materials. Mechanical property changes in irradiated materials are modeled by dislocation dynamics simulations, which simulate a collective motion of dislocations that interact with the defects. In this paper, we present a multi scale modeling methodology that describes reactor pressure vessel embrittlement in a light water reactor environment.

• Journal of Astronomy and Space Sciences
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• 제30권3호
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• pp.133-140
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• 2013

Most of high energy cosmic rays (CRs) are thought to be produced by diffusive shock acceleration (DSA) at supernova remnants (SNRs) within the Galaxy. Fortunately, nonthermal emissions from CR protons and electrons can provide direct observational evidence for such a model and place strong constraints on the complex nonlinear plasma processes in DSA theory. In this study we calculate the energy spectra of CR protons and electrons in Type Ia SNRs, using time-dependent DSA simulations that incorporate phenomenological models for some wave-particle interactions. We demonstrate that the time-dependent evolution of the self-amplified magnetic fields, Alfv$\acute{e}$nic drift, and escape of the highest energy particles affect the energy spectra of accelerated protons and electrons, and so resulting nonthermal radiation spectrum. Especially, the spectral cutoffs in X-ray and ${\gamma}$-ray emission spectra are regulated by the evolution of the highest energy particles, which are injected at the early phase of SNRs. Thus detailed understandings of nonlinear wave-particle interactions and time-dependent DSA simulations of SNRs are crucial in testing the SNR hypothesis for the origin of Galactic cosmic rays.

• Bulletin of the Korean Chemical Society
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• 제21권8호
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• pp.805-808
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• 2000

Mixed crystal powders based on Cd,Fe, and S have been synthesized by varying the ratio of CdS and $FeS_2in$ order to find a suitable material usefuI for the effectivc conversion of solar energy. Hydrogen gas was evolved only with CdS/Ptby photocatal ytic reaction under white light in an aqueous 1 M sodiumsulfite solution. From electrochemical studies of semiconductor electrodes. itwas shown that the onset potential shifted to the positive direction and that the bandgap energy also decreased as the molar ratio of Fe increased. A hydrogen evolution mechanism in terms of the conduction band potential and hydrogen evolution potential is proposed.

• 공업화학
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• 제34권6호
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• pp.567-575
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• 2023

물의 전기 분해는 효과적인 그린 수소를 생산하기 위한 유망한 기술 중 하나로서 활발한 연구가 이루어지고 있다. 수전해 시스템의 원료로 해수를 직접 사용하게 되면 지구상에 있는 물의 약 97%를 해수가 차지하고 있으므로, 기존 담수 원료의 제한성에 대한 문제를 해결할 수 있다. 동시에 풍부한 부생 원료를 얻을 수 있는데, 그 성분과 pH 환경에 따라 전기 분해 과정에서 생성되는 Cl₂, ClO^-, Br₂ 및 Mg(OH)₂ 등이 대표적이다. 성공적인 해수 수전해 시스템 개발과 이에 필수적인 산소발생반응(oxygen evolution reaction, OER)과 수소발생반응(hydrogen evolution reaction, HER) 촉매를 개발하기 위해서는 해수 환경에서 일어나는 반응의 원인과 결과에 대해 파악할 필요가 있다. 따라서 본 논문에서는 해수 수전해 시스템의 반응 메커니즘과 특징 및 애노드와 캐소드 전극에 사용되는 전기화학 촉매들의 연구 개발 동향에 대해 살펴보고자 한다.

• 천문학회보
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• 제38권2호
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• pp.59.1-59.1
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• 2013

Type Ia supernovae (SNe) are providing the most conclusive evidence for accelerating universe with dark energy in observational cosmology. In these investigations, look-back time evolution of SNe luminosity is regarded as negligible on the basic assumption. However, several recent works present some systematic differences among hosts which have different characteristics of stellar population. For more direct investigation, we are proceeding with our YONSEI (YOnsei Nearby Supernovae Evolution Investigation) project. Only early-type hosts in our catalogue were chosen in order to estimate the luminosity-weighted mean age and metallicity directly using Single Stellar Population (SSP) models and ignore the effect from the dust extinction. Observations using low-resolution spectrographs are still in progress at Las Campanas Observatory with 2.5m telescope and at McDonald Observatory with 2.7m telescope. We have thus far obtained spectra for 30 early-type hosts. After weak emission line correction, Lick/IDS absorption-line indices are measured and YEPS spectroscopic evolution model was applied to determine mean population ages and metallicities. Our preliminary results show that SNe Ia hosted in older galaxies seem to be brighter at 1.4 - 3 sigma levels, however, more observations and analyses are still needed to confirm this correlation.

• 천문학회지
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• 제40권4호
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• pp.161-164
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• 2007

We calculate the evolution of multiple supernova (SN) explosions inside a pre-exiting bubble blown up by winds from massive stars, using one-dimensional hydrodynamic simulations including radiative cooling and thermal conduction effects. First, the development of the wind bubble driven by collective winds from multiple stars during the main sequence is calculated. Then multiple SN explosion is loaded at the center of the bubble and the evolution of the SN remnant is followed for $10^6$ years. We find the size and mass of the SN-driven shell depend on the structure of the pre-existing wind bubble as well as the total SN explosion energy. Most of the explosion energy is lost via radiative cooling, while about 10% remains as kinetic energy and less than 10% as thermal energy of the expanding bubble shell. Thus the photoionization and heating by diffuse radiation emitted by the shock heated gas is the most dominant form of SN feedback into the surrounding interstellar medium.

• 천문학논총
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• 제30권2호
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• pp.69-71
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• 2015

In our previous work, we investigated the orbital dynamics of Asteroid 1934 CT (or 1989 AC or 4179 Toutatis) from epoch 2012-Jul-24 (JDE2456132.5) using the Mercury program package. Asteroid 4179 Toutatis has an Earth and Mars crossing orbit with semimajor axis a = 2.5292 AU and eccentricity e = 0.6294, and therefore the perihelion distance is q = 0.9373 AU and the aphelion distance is Q = 4.1211 AU. After more than 300,000 years, asteroid 4179 Toutatis will escape from the Solar System, but during this time, it will have close-encounters with other planets from Venus to Uranus. As a continuation of this project, we investigated its energy changes in each close encounter. We also determine the energy of this asteroid when it escapes from the Solar System. The result is that during its orbital evolution, the energy of this asteroid changes and gives us negative, zero and positive values.

• 천문학회보
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• 제38권2호
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• pp.51.2-51.2
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• 2013

Galactic fly-by interactions are believed to be far more frequent than direct mergers, acting as hidden drivers of galaxy evolution. We perform a tree-particle-mesh code GOTPM, and investigate the statistical properties of the fly-by interactions as functions of halo masses and ambient environments. Based on the total energy of the two halos of interest, impulsive fly-by pairs are identified from eventual merger candidates. We find three obvious results as follows: (1) Halos in the high-dense environment experience more frequent mergers and fly-by encounters than those in the low-dense region; (2) In the massive halos, both merger and fly-by fractions evolve more dramatically with time than those in dwarfs; and (3) The fly-by fraction decreases as approaching the present epoch, in contrast to the increase of the merger fraction.