• 자동차안전학회지
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• 제7권2호
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• pp.8-14
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• 2015

The objective of this study was to construct the spring-mass models for the car-to-car frontal impact crash. The SISAME software was utilized to extract the spring-mass models using the data from US-NCAP frontal crash tests. The spring-mass models of a compact car and a midsize car could effectively approximate the crash characteristics for the full frontal barrier impact and the car-to-car frontal impact scenarios. Compared to the barrier crash tests, the dummy injuries of midsize car decreased, while the dummy injuries of compact car increased, under the frontal car-to-car crash circumstances.

• 대한기계학회논문집B
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• 제24권5호
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• pp.668-676
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• 2000

A two-dimensional model for pulse tubes with tapered cross-section was proposed. Net enthalpy flow and steady mass streaming were investigated by two-dimensional analysis of mass, momentum and energy equations of the gas as well as energy conservation of the tube wall. Steady mass flux profiles show good agreement with the previous approximate solution. It was shown that steady mass streaming can be reduced by tapering a pulse tube and by increasing the length of a pulse tube. Effects of the velocity phase angle and frequency on steady mass streaming were shown.

• Advances in environmental research
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• 제5권4호
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• pp.213-224
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• 2016

This paper presents a numerical model based on a UTCHEM simulator to simulate surfactant flushing process to remediate diesel contaminated sand column. For this purpose, we modeled remediation process under 10000 and 20000 ppm initial concentrations of diesel. Various percent-mass sodium dodecyl sulfate (SDS) considered in our model. The model results indicated that 0.3 percent-mass of SDS at 10000 ppm and 0.1 percent-mass of SDS at 20000 ppm initial diesel concentration had maximum removal perdition which is in agreement with the experiment results. For 10000 ppm diesel concentrations, the coefficient of determination ($R^2$) and index of agreement (IA) between the model result and the experimental data were 0.9952 and 0.9695, respectively, and for 20000 ppm diesel concentrations, $R^2$ and IA were 0.9977 and 0.9935, respectively. The sensitivity analysis of permeability illustrated that in all diesel concentrations and SDS percent-mass with increasing permeability the model resulted in more removal efficiency.

• 천문학회지
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• 제46권6호
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• pp.235-242
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• 2013

We compare mass-loss rates of OH/IR stars obtained from radio observations with those derived from the dust radiative transfer models and IR observations. We collect radio observational data of OH maser and CO line emission sources for a sample of 1533 OH/IR stars listed in Suh & Kwon (2011). For 1259 OH maser, 76 CO(J=1-0), and 55 CO(J=2-1) emission sources, we compile data of the expansion velocity and mass-loss rate. We use a dust radiative transfer model for the dust shell to calculate the mass-loss rate as well as the IR color indices. The observed mass-loss rates are in the range predicted by the theoretical dust shell models corresponding to $\dot{M}=10^{-8}M_{\odot}/yr-10^{-4}M_{\odot}/yr$. We find that the dust model using a simple mixture of amorphous silicate and amorphous $Al_2O_3$ (20% by mass) grains can explain the observations fairly well. The results indicate that the dust radiative transfer models for IR observations generally agree with the radio observations. For high mass-loss rate OH/IR stars, the mass-loss rates obtained from radio observations are underestimated compared to the mass-loss rates derived from the dust shell models. This could be because photon momentum transfer to the gas shell is not possible for the physical condition of high mass-loss rates. Alternative explanations could be the effects of different dust-to-gas ratios and/or a superwind.

• Journal of Astronomy and Space Sciences
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• 제3권2호
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• pp.103-116
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• 1986

The mass distribution and other related quantities were calculated by fitting the observed rotation curve(Davoust and de Vaucouleur 1980) to Brandt and Belton's mass distribution model. One of n values for mass model is determined as 1.5(Vm=95 $kms^{-1}$) and two pairs of them are determined as 0.8(Vm = 95$kms^{-1}$) and 2.0 and 0.8 (Vm = 55$kms^{-1}$) and 2.0 because of the hump in observed rotation curve. Total masses and integrated mass to luminosity ration are $1.8\times10^{10}M_\odot,\;1.5\times10^{10}M_\odot,\;1.4\times10^{10}M_\odot$, and 6.57, 5.33, 5.26 for three cases according to n values. Integrated mass to luminosity ratio in Holmberg radius is 3.44, 3.26, 3.00 in god agreement with the typical value of Sd type suggested by Faber and Gallagher(1979). Presented halo masses which are fifty percent of total masses and halo mass to luminosity ratios given as 75.83, 53.50, 58.75 are values less than Turner's(1976).

• 한국공간구조학회논문집
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• 제18권2호
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• pp.43-50
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• 2018

In this study, TMD(Tuned Mass Damper) is installed in a retractable-roof spatial structure in order to investigate dynamic response characteristics according to mass ratio and installed position of TMD on large spatial structures. The example analytical model is generated based on the Singapore sports hub stadium. Twenty eight analytical models are used to investigate optimal installation position of TMD for the example retractable-roof spatial structure using 4 to 16 TMDs. The mass of one TMD is set up 1% of total mass at the example analytical model. Displacement response ratio of model with TMD is compared with that of base model without TMD. It has been found from numerical simulation that it is more effective to install TMD at the edge of the spatial structure rather than to concentrate the TMD at the center of the spatial structure.

• 폴리머
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• 제28권2호
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• pp.121-127
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• 2004

폴리(에틸렌 나프탈레이트)의 축중합 반응은 가역반응이므로 부반응 물질인 에틸렌 글라이콜의 신속한 제거가 높은 분자량의 제품을 얻는데 매우 중요하다. 본 연구에서는 폴리(에틸렌 나프탈레이트)올리고머로 박막을 제조하여 실제 반응기와 동일한 조건 하에서 (28$0^{\circ}C$, <0.1mmHg) 반응시켜 이 때 일어나는 물질 전달 현상을 관찰하고자 하였다. 여러 가치 두께의 박막을 제조하여 반응 실험한 결과 두께가 0.025cm 이하의 영역에서는 박막에서의 물질 전달 저항이 크지 않아 총괄 반응 속도에 영향을 미치지 않음을 관찰하였다. 물질 전달 모델 및 확산 모델을 사용하여 반응 결과를 예측한 결과 두 모델 모두 실험 결과를 잘 예측하였으나 확산 모델의 경우 중합도가 낮은 영역에서 물질 전달 모델에 비해 반응이 더 빨리 진행되는 경향을 보였다. 두 모델을 이용하여 물질 전달 관련 계수를 예측한 결과 폴리(에틸렌 나프탈레이트)에서의 확산 계수는 4.7${\times}$$10^{-6}$$\textrm{cm}^2$/sec, 물질 전달 계수는 1.4${\times}$$10^{-4}$cm/sce로 폴리(에틸렌 테레프탈레이트) 경우보다 작은 값을 보였다.

• 천문학회보
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• 제36권2호
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• pp.53.2-53.2
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• 2011

We combine the physics of the ellipsoidal collapse model with the excursion set theory to study the shapes of dark matter halos. In particular, we develop an analytic approximation to the nonlinear evolution that is more accurate than the Zeldovich approximation; we introduce a planar representation of halo axis ratios, which allows a concise and intuitive description of the dynamics of collapsing regions and allows one to relate the final shape of a halo to its initial shape; we provide simple physical explanations for some empirical fitting formulae obtained from numerical studies. Comparison with simulations is challenging, as there is no agreement about how to define a non-spherical gravitationally bound object. Nevertheless, we find that our model matches the conditional minor-to-intermediate axis ratio distribution rather well, although it disagrees with the numerical results in reproducing the minor-to-major axis ratio distribution. In particular, the mass dependence of the minor-to-major axis distribution appears to be the opposite to what is found in many previous numerical studies, where low-mass halos are preferentially more spherical than high-mass halos. In our model, the high-mass halos are predicted to be more spherical, consistent with results based on a more recent and elaborate halo finding algorithm, and with observations of the mass dependence of the shapes of early-type galaxies. We suggest that some of the disagreement with some previous numerical studies may be alleviated if we consider only isolated halos.

• 한국지구과학회지
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• 제35권5호
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• pp.362-374
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• 2014

This study investigated the initial mass function (IMF) and star formation history of high-mass stars in the Small Magellanic Cloud (SMC) using a population synthesis technique. We used the photometric survey catalog of Lee (2013) as the observable quantities and compare them with those of synthetic populations based on Bayesian inference. For the IMF slope (${\Gamma}$) range of -1.1 to -3.5 with steps of 0.1, five types of star formation models were tested: 1) continuous; 2) single burst at 10 Myr; 3) single burst at 60 Myr; 4) double bursts at those epochs; and 5) a complex hybrid model. In this study, a total of 125 models were tested. Based on the model calculations, it was found that the continuous model could simulate the high-mass stars of the SMC and that its IMF slope was -1.6 which is slightly steeper than Salpeter's IMF, i.e., ${\Gamma}=-1.35$.

• Journal of Astronomy and Space Sciences
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• 제9권1호
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• pp.11-29
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• 1992

In 1963, Toomre built up classes of mass models for the highly flattened galaxies which have free parameters n, $a_n$ and $C_n$. In order to keep the universal dimension, we adopt parameters $b_n({C_n}^2={a_n}^{2n}+^2{b_n}^2/(n-1)!)$ insteal of $C_n$. Series of the normalized Toomre's mass models (G = $V_{max}$ =$R_{max}$ = 1, n = 1 to 7) are derived and the normalized parameters $a_n$ and $b_n$ are determined by the iteration method. Replacing parameters $a_n$ and $b_n$ to ${a_n}^l(=a_nr_{max})$ and ${b_n}^l(=b_n\cdotV_{max}/r_{max})$, we can get the generalization of Toomre's mass model.