• Environmental Engineering Research
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• v.24 no.3
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• pp.382-388
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• 2019

Although nanobubbles attract significant attention, their characteristics and applications have not been thoroughly defined. There are diverse opinions about the definition of nanobubbles and controversy regarding methods that verify their characteristics. This study defines nanobubbles as having a size less than $1{\mu}m$. The generation of these sub-micron (nano) bubbles may be verified by induced coalescence or light scattering. The size of a sub-micron (nano) bubbles may be measured by optical, and confocal laser scanning microscopy. Also, the size may be estimated by the relationship of bubble size with the dissolved oxygen concentration. However, further research is required to accurately define the average bubble size. The zeta potential of sub-micron (nano) bubbles decreases as pH increases, and this trend is consistent for micron bubbles. When the bubble size is reduced to about 700-900 nm, they become stationary in water and lose buoyancy. This characteristic means that measuring the concentration of sub-micron (nano) bubbles by volume may be possible by irradiating them with ultrasonic waves, causing them to merge into micron bubbles. As mass transfer is a function of surface area and rising velocity, this strongly indicates that the application of sub-micron (nano) bubbles may significantly increase mass transfer rates in advanced oxidation and aeration processes.

• 한국신재생에너지학회:학술대회논문집
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• 2007.06a
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• pp.172-175
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• 2007

The Performance of a PEMFC stack is strongly dependent on the uniform reactants distribution on MEA. The uniform distribution can be achieved by flow-field pattern and manifold design optimized to satisfy operating conditions. This paper investigates uniform reactants distribution in channels by changing manifold shape and inlet mass flow rate. Typical U and Z shape and modified U and Z shape manifolds with buffer zone were designed. To check the uniform reactants distribution, standard deviation of mass flow rate was compared. The numerical results show that the inlet mass flow rate, inlet shape, and manifolds shape are critical factor for uniform distribution.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.1
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• pp.72.1-72.1
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• 2018

Recently, an analysis of 3-micron spectra of CH4 line emission from our Gemini/GNIRS observations of Jupiter's polar regions yielded an unexpected result: The homopause (~1 microbar pressure level) located directly above the long-lasting 8-micron CH4 north-polar hot spot (Great 8-micron Hot Spot: GHS) is cool compared with the temperatures of nearby auroral regions (Kim et al. 2017). Most of the 8-micron emission of the GHS originates from CH4 at the ~1 mbar level (i.e., deeper in the stratosphere, where cooling time is several years), much longer than at the altitude of the homopause. We propose a mechanism to explain the temperature difference: locally-fixed and transient, but energetic auroral particles, which can penetrate to the 1 mbar level and deposit energy there creating and maintaining the GHS. For Saturn, thus far we have not detected distinctive 8-micron nor 3-micron CH4 hot spots in the polar regions. We will present a possible implication for this difference between Jupiter and Saturn.

• The Bulletin of The Korean Astronomical Society
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• v.44 no.2
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• pp.44.3-44.3
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• 2019

Since the detection of 3.3-micron PAH (polycyclic aromatic hydrocarbon) and 3.4-micron aliphatic hydrocarbon features in the spectra of Titan (Bellucci et al. 2009; Kim et al. 2011) and Saturn (Kim et al. 2012), respectively, the 3.3-micron feature of gaseous CH4 has been thought to be still the important spectral feature in the 3-micron absorption structures of Titan and Saturn. However, the analyses of the 3.3-and 3.4-micron emission structures of Saturn revealed that the influence of the gaseous CH4 on the structures is rather minimal (Kim et al. 2019). We present synthetic spectra of gaseous CH4, and the PAH and aliphatic haze particles in order to show the degree of influence of their spectra on the 3.3-and 3.4-micron emission structures of Saturn, and we compare these synthetic spectra with currently available observations. We constructed these synthetic spectra using newly developed radiative transfer equations. These equations are able to address detailed radiative processes in the atmospheres containing various gases and haze particles. We expect these radiative transfer equations can also be widely applied to the investigation of radiative transfer processes and the analyses of the spectra of celestial objects such as the Earth, the Moon, planets, and interstellar nebulae.

• Proceedings of the Korean Institute of Electrical and Electronic Material Engineers Conference
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• 1995.11a
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• pp.232-235
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• 1995

To improve the DIBL characteristics of deep sub micron BC PMOSFETs, the methods of DCI(Deep Channel Implantation) and Hale Implantation have been reported. In this study, using the process simulator TSUPREM4, we simulated the 0.25$\mu\textrm{m}$ and 0.45$\mu\textrm{m}$ gate length BC PMOSFETs applying the both methods to improve the DIBL characteristics, and their electric characteristics were compared to find the mothod suitable far deep sub-half micron BC PMOSFETs, using the device simulator MEDICI. So we found out that the method of Halo Implantation could be applied to deep sub-half micron BC PMOSFETs for 255 Mbit DRAM.

• The Bulletin of The Korean Astronomical Society
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• v.44 no.1
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• pp.55.1-55.1
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• 2019

Recently, temporal variations of the 3-micron emissions of methane and ethane have been detected in the auroral regions of Jupiter observed from Gemini North (Kim et al. 2019, in preparation). These temporal variations of 3-micron hydrocarbon emissions in the auroral regions can be caused by the following phenomena: temporal variations of temperatures, mixing ratios, auroral particle bombardments and Joule heatings, and the combinations of these. Although we are not able to quantitatively determine the cause of the temporal variations at this moment, we will present the following quantitative discussions: thermal influences on the 3-micron emissions, global mixing ratio distributions of the hydrocarbon molecules, and energy distributions of auroral particles penetrating the hydrocarbon layers. We will also present a possible correlation between the temporal variations of the 3-micron emissions and solar wind activities.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.2
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• pp.74.1-74.1
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• 2011

To probe the connection between starburst and AGN activity, we investigate the relation between the 3.3 micron~PAH emission and AGN properties based on the new AKARI observations and the data collected from the literature. Using a sample of low-z Type I AGN, we measure the global 3.3 micron PAH luminosity from the AKARI slit-less spectroscopy. The 3.3 ${\backslash}$micron~PAH emissions are detected for 7 out of 26 target galaxies, but we find no strong correlation between the 3.3 ${\backslash}$micron~PAH emission and AGN luminosity, suggesting that global star formation may not be tightlyrelated with AGN activity. In contrast the to global star formation, the nuclear 3.3 micron~PAH emission luminosity, which are measured from ground-based long slit spectroscopy with a narrow slit, correlates with AGN luminosity. These results imply that starburst and AGN activity are directly connected at the nuclear region.

• Journal of the Korean Ceramic Society
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• v.33 no.5
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• pp.547-555
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• 1996

Porous alumina ceramics were fabricated by pseudo-boehmite phydosol-gel process within/without commercial $\alpha$-alumina particles average 1 and 40 micron respectively. The pore characteristics of fired specimens were studied by the measurement of bulk density total porosity thyermal analysis pore volume pore distribution BET area XRD and SEM. with increasing of firing temperature pore volume and BET surface area were decreased and the average pore size was increased to approximately 146$\AA$ upto 80$0^{\circ}C$ by de-watering of [OH] and formation of $\alpha$-alumina. The fired relative density of the alumina-dispersed specimen with average 1 micron particle was increased with the amounts of dispersed particle by bimodal packing theory which is compared to the ones of specimen including of average 40 micron particle. It was confirmed that the percola-tion threshold in porous ceramics with coarser particle (40 micron) has formed between the transformed-alumina from hydrogel and dispersed-alumina of above 50 vol% particle and the total porosity was increased at the threshold point above.

• Proceedings of the Materials Research Society of Korea Conference
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• 2009.05a
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• pp.50.2-50.2
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• 2009

사파이어는 질화물계 광전자소자 제작 시 박막 성장 기판으로 주로 사용되어 최근 그 중요성이 부각되고 있다. 특히 미세 패턴이 형성된 사파이어 기판을 이용하여 질화물계 발광다이오드 소자를 제작하면 빛의 난반사가 증가하여 광추출효율에 큰 개선이 나타난다. 또한 사파이어는 화학적 안정성이 뛰어나고, 높은 강도를 지녀 나노임프린트 등 여러 가지 패터닝 공정에서 패턴 형성 몰드로도 응용될 수 있다. 그러나 이와 같은 사파이어의 화학적 안정성으로 인하여 sub-micron 크기의 미세 패턴을 형성하기 힘들며, 현재 사파이어의 패턴은 micron 크기로 제한되어 사용되고 있다. 본 연구에서는 나노임프린트 리소그라피(NIL)를 사용하여 사파이어 웨이퍼의 c-plane위에 sub-micron 크기의 hole 패턴 및 pillar 패턴을 형성하였다. 우선 Hole 패턴을 형성하기 위해 사파이어 기판 위에 금속 hard mask 패턴을 UV 임프린트 공정과 etch 공정을 통해 형성하였다. 그리고 이 금속 패턴을 mask로 사파이어를 ICP 식각을 하여 hole 패턴을 형성하였다. 또한 Pillar 패턴을 형성하기 위해 lift-off 공정을 이용하여 금속 마스크 패턴을 형성하였고 이를 ICP 식각을 통해 사파이어 기판 위에 pillar 패턴을 형성하였다.

• Proceedings of the Materials Research Society of Korea Conference
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• 1994.11a
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• pp.186-187
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• 1994