• 천문학회지
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• 제34권4호
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• pp.333-335
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• 2001

We study the properties of supernova (SN) driven interstellar turbulence with a numerical magnetohydrodynamic (MHD) model. Calculations were done using the RIEMANN framework for MHD, which is highly suited for astrophysical flows because it tracks shocks using a Riemann solver and ensures pressure positivity and a divergence-free magnetic field. We start our simulations with a uniform density threaded by a uniform magnetic field. A simplified radiative cooling curve and a constant heating rate are also included. In this radiatively-cooling magnetized medium, we explode SNe one at a time at randomly chosen positions with SN explosion rates equal to and 12 times higher than the Galactic value. The evolution of the system is basically determined by the input energy of SN explosions and the output energy of radiative cooling. We follow the simulations to the point where the total energy of the system, as well as thermal, kinetic, and magnetic energy individually, has reached a quasi-stationary value. From the numerical experiments, we find that: i) both thermal and dynamical processes are important in determining the phases of the interstellar medium, and ii) the power index n of the $B-p^n$ relation is consistent with observed values.

• 천문학회지
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• 제19권1호
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• pp.33-49
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• 1986

Radial distribution of internal density has been determined for thirteen subclouds in the three giant molecular cloud complexes accompanying Mon OB1, Mon OB2 and CMa OB1 associations, We modeled their radial density structures with the density distribution of isothermal gas spheres. Most of the subclouds, nine out of the thirteen, are well described by isothermal spheres of single component; while the rest four require an additional component. Total mass and potential energy of each subcloud are also derived from the radial density structure; thermal energy and internal velocity dispersion required for sustaining the density structure are deduced from the isothermal gas model. Our derived masses of the clouds are comparable to the values determined by Blitz (1978) under LTE assumption. This agreement suggests that the correction factor for non-LTE effect on mass-estimate is not far from unity. The ratio of the gravitational potential energy to the kinetic energy of thermal motion is as large as 250; hence the thermal motion alone cannot support these clouds against the gravity. Being supported by turbulence motion with velocities of six to seven times the thermal velocity, the clouds of one-component type seem to be in equilibrium with the gravity; while the clouds of two-component type are likely to be in the stage of gravitational collapse.

• Computers and Concrete
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• 제30권1호
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• pp.19-32
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• 2022

This paper presents an investigation into the failure of RC columns under impact loadings. A numerical simulation of 19 identical RC columns subjected to single and repeated impact loadings was performed. A free-falling hammer was dropped at midspan with the same total kinetic energy input but varying mass and momentum. The specimens under the repeated impact test were struck two times at the same location. The colliding index, defined as the impact energy-momentum ratio, was proposed to explain the different impact responses under equal-energy impacts. The increase of colliding index from low to high indicates the transition of the impact response from static to dynamic and failure mode from flexure to shear. This phenomenon was more evident when the column had a greater axial load and was impacted with a high colliding index. The existence of the axial load had an inhibitory effect on the crack development and increased the shear resistance. The second impact changes the failure mode from flexural to brittle shear as found in the specimen with 20% axial load subjected to high a colliding index. Moreover, a deflection prediction equation based on the impact energy and force was limited to the low colliding index impact.

• 한국식품위생안전성학회지
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• 제37권3호
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• pp.173-180
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• 2022

오징어의 품질을 평가하기 위한 여러 항목 들이 있으나 현장에서 소비자 및 유통업자들의 경우 주관적인 관능평가에 의존하고 있으며 소비자의 어류 구매의사 결정에 부패취가 직접적인 영향을 미칠 수 있다. 따라서 관능적 평가를 입증 할 수 있는 과학적인 품질인자를 제시하고자 하였으며, 온도와 저장시간에 따른 상호관계를 분석하였다. 과학적 품질인자로는 TVC, Pseudomonas spp., pH, VBN 으로 선정하였으며 세 가지 온도 조건에서 보관하였다. 이취발생검지시점은 R-index를 이용해 측정하고 kinetic 모델링을 진행하였다. 모델링 결과 활성화 에너지는 이취발생검지 시간이 51.210 kJ/mol, TVC는 42.888 kJ/mol, Pseudomonas spp.는 50.283 kJ/mol, VBN은 72.594 kJ/mol, pH는 41.990kJ/mol 으로 나타났다. Pseudomonas spp., TVC, pH, VBN 순으로 이취발생검지 시간의 활성화 에너지에 근사하였으며, 특히 Pseudomonas spp.는 이취발생검지 시간의 활성화 에너지와 가장 유사하였다. 따라서 오징어의 이취발생 indicator는 이취발생시간과 가장 유사한 양상을 나타내는 Pseudomonas spp.로 판단 할 수 있었다.

• Bulletin of the Korean Chemical Society
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• 제31권5호
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• pp.1295-1300
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• 2010

The $CO_2-CH_4$ reaction catalyzed by Ni/silicon wafers was kinetically studied by using a photoacoustic technique. The catalytic reaction was performed at various partial pressures of $CO_2$ and $CH_4$ (50 Torr total pressure of $CO_2/CH_4/N_2$) in the temperature range of 500 - $650^{\circ}C$ in a static reactor system. The photoacoustic signal that varied with the $CO_2$ concentration during the catalytic reaction was recorded as a function of time. Under the reaction conditions, the $CO_2$ photoacoustic measurements showed the as-prepared Ni thin film sample to be inactive for the reaction, while the $CO_2/CH_4$ reactions carried out in the presence of the sample pre-treated in $H_2$ at $600^{\circ}C$ were associated with significant time-dependent changes in the $CO_2$ photoacoustic signal. The rate of $CO_2$ disappearance was measured from the $CO_2$ photoacoustic signal data in the early reaction period of 50 - 150 sec to obtain precise kinetic data. The apparent activation energy for $CO_2$ consumption was determined to be 6.9 kcal/mol from the $CO_2$ disappearance rates. The partial reaction orders, determined from the $CO_2$ disappearance rates measured at various $PCO{_2}'S$ and $PCH{_4}'S$ at $600^{\circ}C$, were determined to be 0.33 for $CH_4$ and 0.63 for $CO_2$, respectively. Kinetic data obtained in these measurements were compared with previous works and were discussed to construct a catalytic reaction mechanism for the $CO_2-CH_4$ reaction over Ni/silicon wafer at low pressures.

• 방사성폐기물학회지
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• 제4권3호
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• pp.209-216
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• 2006

중성자가 조사된 흑연에 내재되어 있는 Wigner 에너지를 배출시키는 방법의 하나인 가열냉각공정의 적용 예로 DSC(미분 주사선 열량계) 측정을 통해 흑연으로부터 Wigner 에너지가 배출되는 열 배출 특성을 연구하였다. 일정온도 상승 방법 에 의한 DSC 운전에서 중성자가 조사된 흑연을 가열냉각(annealing)하는 동안 배출되는 Wigner 에너지의 총량과 처리온도에 따른 배출속도를 측정하였다. 연구로 2호기(KRR-2) thermal column 내에 위치별로 중성자의 조사량에 차이가 나는 흑연 시료를 분말로 만들어 상온에서 $500^{\circ}C$까지의 온도 범위에서 DSC를 운전하고 이로부터 Wigner 에너지의 배출 속도를 측정하였다. 가열냉각 동안 중성자가 조사된 흑연에서 배출되는 Wigner 에너지의 배출 특성은 가변적 활성화 에너지 속도 식으로 잘 상관시킬 수 있었다.

• 대기
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• 제26권3호
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• pp.401-412
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• 2016

A 3D sonic anemometer has been installed at Yongpyong alpine slope since Oct. 23th 2014 to observe the slope winds and to analyze turbulent characteristics with the change in surface cover (grass and snow) and the synoptic wind strength. Eddy covariance method has been applied to calculate the turbulent quantity after coordinate transformation of a planar-fit rotation. We have carefully selected 3 good episodes in the winter season (23 October 2014 to 28 February 2015) for each category (9 days in total), such as grass and snow covers in case of weak synoptic wind condition, and grass cover of strong synoptic wind. The diurnal variations of the slope winds were well developed like the upslope wind in the daytime and downslope wind in the nighttime for both surface covers (grass and snow) in the weak synoptic forcing, when accordingly both heat and momentum fluxes significantly increased in the daytime and decreased in the nighttime. Meanwhile, diurnal variation of heat flux was not present on the snow cover probably in associated with significant fraction of sunlight reflection due to high albedo especially during the daytime in comparison to those on the grass cover. In the strong synoptic regime, the most dominant feature at Yongpyong, only the southeasterly downslope winds were steadily generated irrespective of day and night with significant increases in momentum flux and turbulent kinetic energy as well, which could suggest that local circulations are suppressed by the synoptic scale forcing. In spite of only one season analysis applied to the limited domain, this kind of an observation-based study will provide the basis for understanding of the local wind circulation in the complex mountain domain such as Gangwon in Korea.

• 공업화학
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• 제30권2호
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• pp.190-197
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• 2019

활성탄을 사용하여 수용액으로부터 메틸 그린 염료의 흡착에 대해 초기농도와 접촉시간 및 온도를 흡착변수로 사용하여 조사하였다. 흡착평형관계는 Freundlich 등온식에 잘 맞았다. 평가된 Freundlich 분리계수(1/n = 0.212~0.305)로부터 이 흡착공정이 효과적인 처리영역(0 < $R_L$ < 1)에 속하는 것을 알았다. BET식으로부터 얻은 등온포화용량은 온도가 증가할수록 커졌다. Dubinin-Radushkevich식으로 구한 흡착에너지값(E = 316.869~340.049 J/mol)으로부터 흡착공정이 물리흡착공정임을 알았다. 흡착속도실험결과는 유사 2차 반응속도식에 잘 맞는 것으로 나타났다. 자유에너지(-5.421~-7.889 kJ/mol)와 엔탈피(31.915 kJ/mol)는 흡착공정이 자발적이고 흡열반응으로 진행되었다고 알려주었다. 등량흡착열은 평형흡착량이 증가함에 따라 커졌으며, 표면 덮임이 증가됨에 따라 흡착제-흡착질의 총 상호작용도 증가하였다.

• 대한기계학회논문집
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• 제9권6호
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• pp.714-724
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• 1985

본 논문에서는 입자가 부상된 2상유동의 해석에서 여러유동조건의 유동을 공 통적으로 해석할 수 있고 또 유동의 난류구조를 규명할 수 있도록 하기 위해서 2-방정 식 난류모델을 적용하였고 또 지배방정식들 속에 나타나는 1유체와 2유체의 2차 상관 관계들을 모형화 할 때 Taweel and Landau의 스펙트럼 이론을 확장발전시켜 적용하였 다.

• 천문학회지
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• 제51권2호
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• pp.37-48
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• 2018

Massive stars blow powerful stellar winds throughout their evolutionary stages from the main sequence to Wolf-Rayet phases. The amount of mechanical energy deposited in the interstellar medium by the wind from a massive star can be comparable to the explosion energy of a core-collapse supernova that detonates at the end of its life. In this study, we estimate the kinetic energy deposition by massive stars in our Galaxy by considering the integrated Galactic initial mass function and modeling the stellar wind luminosity. The mass loss rate and terminal velocity of stellar winds during the main sequence, red supergiant, and Wolf-Rayet stages are estimated by adopting theoretical calculations and observational data published in the literature. We find that the total stellar wind luminosity due to all massive stars in the Galaxy is about ${\mathcal{L}}_w{\approx}1.1{\times}10^{41}erg\;s^{-1}$, which is about 1/4 of the power of supernova explosions, ${\mathcal{L}}_{SN}{\approx}4.8{\times}10^{41}erg\;s^{-1}$. If we assume that ~ 1 - 10 % of the wind luminosity could be converted to Galactic cosmic rays (GCRs) through collisonless shocks such as termination shocks in stellar bubbles and superbubbles, colliding-wind shocks in binaries, and bow-shocks of massive runaway stars, stellar winds might be expected to make a significant contribution to GCR production, though lower than that of supernova remnants.