• 한국정보통신학회논문지
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• 제23권10호
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• pp.1216-1227
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• 2019

본 논문에서는 IoT 서비스 개발 과정에서 효율적인 IoT 애플리케이션 테스팅이 가능하도록 지원하는 도구인 TITAN(Tool for IoT ApplicatioN testing)을 제안한다. TITAN은 IoT 서비스 개발자가 개발 중인 애플리케이션 로직을 테스팅 하는 데 필요한 물리적 환경 및 사용자 행동에 제약받지 않고, 개발 환경에서 애플리케이션 실행 및 확인이 가능하도록 고안되었다. 개발자는 TITAN을 이용하여 개발 과정에서 반복적인 테스팅에 소모되는 시간과 노력을 줄일 수 있을 것이다. 본 논문에서는 TITAN의 시스템 아키텍처와 현재까지 구현된 프로토타입을 제시한다. 또한 소규모 유저 스터디를 통해 TITAN의 유용성과 사용성을 평가한다. 유저 스터디 참가자들은 TITAN의 유용성에 대해 긍정적으로 생각하였다. 마지막으로 현재 연구의 한계와 향후 연구 방향에 대해서 논의한다.

• 천문학논총
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• 제19권1호
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• pp.39-46
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• 2004

We have carried out the high-resolution spectroscopic observations of Titan using BOES (Bohyunsan Echelle Spectrometer) to establish a standard spectral atlas of Titan. The observations were made on November 3, 4, 16 and 17, 2003 using a 300 11m fiber optics with a spectral resolving power of 30,000. The spectral atlas will be served as a reference for the future spectroscopic researches of Titan and other planetary objects. We were able to confirm $CH_4$ absorption lines of the Kuiper bands, and find unidentified lines near $7500{\AA}$.

• 대한화학회지
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• 제58권2호
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• pp.205-209
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• 2014

Hematite iron oxide (${\alpha}$-$Fe_2O_3$) nanowalls were fabricated on aluminum substrate by a facile solvent-assisted hydrothermal oxidation process. The XRD and EDS patterns indicate that the sample has a rhombohedral phase of hematite $Fe_2O_3$. FE-SEM, TEM, HR-TEM, SA-ED were employed to characterize the resulting materials. $N_2$ adsorption-desorption isotherms was used to study a BET surface area. Their capability of catalytic degradation of titan yellow GR azo dye with air oxygen in aqueous solution over $Fe_2O_3$ catalysts was studied. The result indicates that the as-prepared product has a high catalytic activity, because it has a larger surface area. Langmuir and Freundlich isotherms of adsorption dye on the catalysts surface were investigated and the decomposition of titan yellow GR follows pseudo-first order kinetic.

• 천문학회보
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• 제40권2호
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• pp.44.2-44.2
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• 2015

Radiative transfer programs have been developed to simulate near-IR spectra of Titan. The formalism of the radiative transfer calculations includes the absorption and emission lines of $CH_4$, $C_2H_2$, $C_2H_6$, and HCN, and continua produced by Titanian haze particles. Absorption and scattering of sunlight by haze particles are considered by employing a two-stream approximation and a spherical-shell model for the atmospheric layers of Titan. Various constraints on the radiative transfer calculations for generating synthetic spectra will be discussed and presented. Several examples of comparisons between the synthetic spectra and recent spectral observations of Titan will also be presented.

• Membrane and Water Treatment
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• 제11권2호
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• pp.97-109
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• 2020

Membrane fouling is the main drawback of membrane technology. Frequent membrane cleaning and membrane replacement are, therefore, required to reduce membrane fouling that causes permeate flux reduction, lower rejection, or higher operating pressure. Studies have proved that the alteration of membrane properties is the key controlling factor in lessening membrane fouling. Among stimuli-responsive membranes, thermo-responsive membrane is the most popular, with a drastic phase transition and swelling-shrinking behavior caused by the temperature change. In this study, the thermo-responsive ability of two commercial membranes, PolyCera® Titan membrane and PolyCera® Hydro membrane, at different temperatures was studied on the antifouling function of the membrane in palm oil mill effluent (POME) treatment. The evaluation of the membrane's thermo-responsive ability was done through three cycles of adsorption (fouling) and desorption (defouling) processes in a membrane filtration process. The experimental result depicted that PolyCera® Hydro membrane had a higher membrane permeability of 67.869 L/㎡.h.bar than PolyCera® Titan membrane at 46.011 L/㎡.h.bar. However, the high membrane permeability of PolyCera® Hydro membrane was compensated with low removal efficiency. PolyCera® Titan membrane with a smaller mean pore size had better rejection performance than PolyCera® Hydro membrane for all tested parameters. On the other hand, PolyCera® Titan membrane had a better hydrodynamic cleaning efficiency than PolyCera® Hydro membrane regardless of the hydrodynamic cleaning temperature. The best hydrodynamic cleaning performed by PolyCera® Titan membrane was at 35℃ with the flux recovery ratio (FRR) of 99.17 ± 1.43%. The excellent thermo-responsive properties of the PolyCera® Titan membrane could eventually reduce the frequency of membrane replacement and lessen the use of chemicals for membrane cleaning. This outstanding exploration helps to provide a solution to the chemical industry and membrane technology bottleneck, which is the membrane fouling, thus reducing the operating cost incurred by the membrane fouling.

• 암석학회지
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• 제26권1호
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• pp.83-91
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• 2017

본 연구에서는 제주도에서 화산분화에 의해 발생 가능한 화쇄류의 영향 범위를 파악하기 위하여 백록담 외륜산 외측 사면 8개 지점에서 새로운 용암돔이 발생하는 것을 가정하고 이 과정에서의 붕괴로 발생 가능한 화쇄류를 수치모의 하였다. 수치모의에는 TITAN2D 수치모의 프로그램을 사용하였다. TITAN2D프로그램에서 화쇄류 흐름의 속도를 제어하는 변수로 사용되는 내부마찰각과 층저마찰각 중 내부마찰각을 $30^{\circ}$, 층저마찰각을 $20^{\circ}$로 설정하였다. 붕괴되는 돔의 높이와 반경, 초기 붕괴 속도, 수치모의 시간 등을 선정하여 총 96개 시나리오에 대하여 수치모의를 실시하였다. 수치모의 결과 돔 붕괴에 의한 화쇄류는 최대 13.4 km까지 도달하여 한라산 정상부 및 제주시와 서귀포시까지 도달하는 것으로 나타났다. 본 연구를 통해 구축된 시뮬레이션 자료들을 이용하여 제주도의 화산 분화 시 발생 가능한 화쇄류의 피해범위 DB를 구축하고 이를 기반으로 재해도를 작성하여 화쇄류로 인한 피해를 최소화하는데 활용할 수 있을 것으로 기대된다.

• 천문학회지
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• 제41권3호
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• pp.65-76
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• 2008

We have investigated the optical properties of the global haze on Titan from spectra recorded between 7100 and $9200{\AA}$, where $CH_4$ absorption bands of various intensities occur. The Titan spectra were obtained on Feb. 23, 2005 (UT), near the times of the Cassini T3 flyby and Huygens probe, using an optical echelle spectrograph (BOES) on the 1.8-m telescope at Bohyunsan Observatory in Korea. In order to derive the optical properties of the haze as a function of altitude, we developed an inversion radiative-transfer program using an atmospheric model of Titan and laboratory $CH_4$ absorption coefficients available from the literature. The derived extinction coefficients of the haze increase toward the surface, and the coefficients at shorter wavelengths are greater than those at longer wavelengths for the 30 - 120 km altitude range, indicating that the Titanian haze becomes optically thin toward the longer wavelength range. Total optical depths of the haze are estimated to be 1.4 and 1.2 for the 7270 - $7360{\AA}$ and 8940 - $9150{\AA}$ ranges, respectively. Based on the Huygens/DISR data set, Tomasko et al. (2005) reported total optical depths of 2.5 - 3.5 at $8290{\AA}$, depending on the assumed fractal aggregate particle model. The total optical depths based on our results are smaller than those of Tomasko et al., but they partially overlap with their results if we consider a large uncertainty from possible variations of the $CH_4$ mixing ratio over Titan's disk. We also derived the single scattering albedo of the haze particles as a function of altitude: it is less than 0.5 at altitudes higher than ${\sim}150\;km$, and approaches 1.0 toward the surface. This behavior suggests that, at altitudes above ${\sim}150\;km$, the average particle radius is smaller than the wavelengths, whereas near the surface, it becomes comparable or greater.

• Bulletin of the Korean Chemical Society
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• 제34권3호
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• pp.759-762
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• 2013

Four prominent features of Titan's haze are found within the '3.4-${\mu}m$' absorption to be uniform with recent vertically resolved Cassini/VIMS spectra. These are absorptions at 2998 $cm^{-1}$ (3.34 ${\mu}m$), 2968 $cm^{-1}$ (3.37 ${\mu}m$), 2927 $cm^{-1}$ (3.42 ${\mu}m$), and 2882 $cm^{-1}$ (3.47 ${\mu}m$). A detailed fitting suggests that the 2998 $cm^{-1}$ feature could originate from amorphous acetonitrile ($CH_3CN$) carrying about 25% of integrated optical depth; the remaining features, which account for 75% of the integrated optical depth, could arise from a distinct triplet (C-H stretching) structure of radiolyzed hydrocarbons. An additional feature was possibly evidenced at altitudes higher than 300 km and attributable to 'polymer-capped' methane ($CH_4$), significantly constraining the chemical composition of organic haze layers under Titan's active radiation field.

• 천문학논총
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• 제11권1호
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• pp.75-90
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• 1996

The vertical distribution of HCN, $HC_3N$ and $C_2N_2$ have been determined from a sequence of Voyager 1 IRIS limb tangent measurements over Titan's north polar region. This sequence yields gas distributions with ${\sim}200\;km$ altitude resolution over the 50-400 km range. The derived mixing ratios of HCN, $HC_3N$ and $C_2N_2$ are $5{\times}10^{-7}$, $7{\times}10^{-8}$ and $8{\times}10^{-9}$, respectively, at 120 km with a factor of 3 uncertainty.

• 해양환경안전학회지
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• 제23권5호
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• pp.574-584
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• 2017

본 논문에서는 보행로봇의 일종인 TITAN-VIII라 불리는 로봇을 이용하여 가장 짧은 경로를 탐색하여 이동하는 방법에 관한 연구를 나타낸다. 보행로봇의 경우 바퀴구동 로봇에 비해 불규칙한 지면 위를 자유로이 이동 가능한 장점 등을 가지고 있는데 반해 이동속도는 바퀴구동 로봇에 비해 느린 편이다. 따라서 본 논문에서는 목적지에 도달하기까지 시간을 최소화하는 최적경로 탐색 제어방법을 제시하였다. 경로를 탐색하기 위해 Dijkstra's algorithm라 불리는 알고리즘을 기반으로 하여 적용하였다. 또한 로봇이 항상 정적인 자세를 유지하는 로봇의 다양한 자세에 대해서도 다루었다. 로봇의 자세제어와 알고리즘을 통하여 로봇의 관절각 결정에 필요한 여러 수학방정식을 제시하였다. 그 후 원하는 궤적으로 로봇이 이동하고 탐색하는 알고리즘을 고안하였고, 제안한 방법의 결과를 실험으로 확인하였다.