• 대한조선학회논문집
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• 제52권6호
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• pp.471-477
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• 2015

When a ship sails in a seaway, the resistance on a ship increases due to incident waves and winds. The magnitude of added resistance amounts to about 15–30% of a calm-water resistance. An accurate prediction of added resistance in waves, therefore, is essential to evaluate the performance of a ship in a real sea state and to design an optimum hull form from the viewpoint of the International Maritime Organization (IMO) regulations such as Energy Efficiency Design Index (EEDI) and Energy Efficiency Operational Indicator (EEOI). The present study considers added resistance problem of AFRAMAX-class tankers with the conventional bow and Ax-bow shapes. Added resistance due to waves is successfully calculated using 1) a three-dimensional time-domain seakeeping computations based on a Rankine panel method (three-dimensional panel) and 2) a commercial CFD program (STAR-CCM+). In the hydrodynamic computations of a three-dimensional panel method, geometric nonlinearity is accounted for in Froude-Krylov and restoring forces using simple wave corrections over exact wet hull surface of the tankers. Furthermore, a CFD program is applied by performing fully nonlinear computation without using an analytical formula for added resistance or empirical values for the viscous effect. Numerical computations are validated through four degree-of-freedom model-scale seakeeping experiments in regular head waves at the deep towing tank of Hyundai Heavy Industries.

• 유기물자원화
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• 제20권4호
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• pp.127-133
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• 2012

소위 '쎔쥐쥐'(SSaM-GG =Smart, Shared, and Mutual- Green Growth)라는 진화된 개념을 지속가능/영속 발전 나아가 안녕성 평가 등에 응용되길 바라며 개발/제안 한다. SSaM-GG는 5개의 알파벳으로 이루어져 있는데 이것들이 뜻하는 것은 '녹, 경, 사, 과, 자'로서, 각각 '환경+보전성, 경제성장성, 사회발전성, 과학기술성, 자율자발성'의 5가지를 뜻한다. 이 5가지 조건은 원래 지속가능한 발전의 3가지 조건(녹, 경, 사)에서 시작되었으나 서로간의 상반/교착현상으로써 완벽한 발전의 지표로서의 부족함이 보임에 과학기술성과 자율자발성을 추가하여 5개축(녹색별; Green Star)으로서 지난 12년간의 관찰/분석/경험 등으로 점차적으로 진화하여 개발되었다.

• 한국컴퓨터정보학회논문지
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• 제18권1호
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• pp.149-156
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• 2013

본 논문에서는 미세먼지를 제거하기 위하여 설계된 Multi Inner Stage(MIS) 사이클론을 대상으로 입자 제거 효율에 대한 모의실험을 수행하고, 실제 입자에 대한 제거 효율을 확인하고자 하였다. 배출부는 -1,000Pa의 음압조건으로 설정하고, 전산유체해석 프로그램인 STAR-CCM+의 난류 모델과 lagrangian method를 이용하여 $5{\mu}m$와 $10{\mu}m$ 입자에 대해 해석을 실시한 결과, 각각 55.7%와 64.1%의 집진효율을 보였다. 해석 결과와 MIS 사이클론 장비의 실제 입자에 대한 제거 효율의 비교를 위하여 열반응기(heat reactor)를 이용해 $SiO_2$ 입자를 생성시켜 실험을 수행하였다. 실제 생성된 $SiO_2$ 입자의 제거 효율 실험에서는 유량에 따라 63~76% 집진효율을 나타냈다. 전자주사현미경(SEM; scanning electron microscope)과 광대역 미세먼지입자 측정기(WAPS; wide range aerosol particle spectrometer)를 이용하여 실제 생성된 $SiO_2$ 입자의 크기는 15~30nm인 것으로 검증하였다. 이에 일반 상용 알루미나 입자($5{\mu}m$, $10{\mu}m$, 그리고 $20{\mu}m$)를 대상으로 MIS 사이클론의 입자 제거효율 실험을 재차 수행한 결과, 76~95% 정도의 제거효율을 보임으로써 유동 해석보다 실제 실험이 더 높은 제거효율을 보인다는 것을 검증하였다.

• 한국과학교육학회지
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• 제42권2호
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• pp.289-309
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• 2022

힉스입자 발견, 블랙홀 이미지 촬영, 외계행성 탐사, 깊은 우주탐사, 중력파 관측 등 최근 천문학은 매우 빠르게 성장하고 있으며, 학생들도 상대적으로 흥미가 높은 분야이다. 본 연구의 목적은 최근 10년간 천문학 연구 저널에서 높은 빈도로 등장한 키워드들과 중고등학교 과학 교육과정에 포함된 천문학 내용 요소를 7개 영역별로 비교하여 천문학 교육과정 개선에 대한 시사점을 얻는 것이다. 우선 선정된 4개 저널-ApJ, ApJL, A&A, MNRAS-에 2011년부터 2020년까지 게재된 모든 논문의 키워드를 R 패키지로 수집하여 연구 동향을 살펴보았다. 교육과정 내용 요소는 7학년부터 12학년 학생이 배우는 과목 중 천문학 내용 요소가 포함된 6개 과목(과학, 통합과학, 지구과학I, 지구과학II, 물리II, 융합과학)의 2015 개정 교육과정 문서에 제시된 내용 체계표, 성취기준, 성취기준해설을 현직 교사들이 코딩한 결과를 종합하여 추출하였다. 연구 결과는 다음과 같다. 첫째, 천문학에서 꾸준하게 많이 등장하는 키워드는 'galaxies: formation, galaxies: active, star: formation, accretion, accretion discs, method: numerical'이다. 둘째, 천문학 교육과정은 모든 학생이 배우는 공통 과학 과목 안에서 'High Energy Astrophysical Phenomena' 영역을 제외한 모든 영역을 포함하도록 구성되었으나 키워드 수준에서 보면 과목별, 학년별 내용 요소 배치와 새롭게 도입할 만한 주제에 대한 검토가 필요한 것으로 나타났다. 본 연구는 과목의 근간을 이루는 과학연구 분야와 교육과정을 비교한 탐색적 연구로서, 연구 결과는 향후 천문학 교육과정 개정에 시사점을 줄 수 있는 기초 연구가 되길 기대한다.

• 천문학회보
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• 제40권1호
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• pp.60.1-60.1
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• 2015

High energy photons and mechanical energy produced by the process of star formation result in copious FIR molecular and atomic lines, which are important coolants of the system. Photons thermally or mechanically induced could dissociate water in the dense envelope to change relative abundances among the species of O, OH, and H2O. Here we analyze OH emission lines toward embedded young stellar objects (YSOs) observed as part of the Herschel open time key program, 'Dust, Ice, and Gas In Time (DIGIT)' in order to study the physical conditions of associated gas and the energy budget loaded on the OH line emission. According to our analysis of the Herschel/PACS spectra, OH emission peaks at the central spaxel in most of sources, but several sources show spatially extended emission structures. In the extended emission sources, the distribution of OH emission is correlated with that of [OI] emission and extended along the outflow directions. Considering the diversity of source properties, ratios between detected OH lines are relatively constant among sources. In addition, each OH line has strong correlation with bolometric luminosity. In order to determine the physical conditions of YSOs, we adopt several methods for the analysis of the OH lines: rotational diagram, non-LTE LVG analysis, and a 2-D PDR code. From the simple LVG analysis, we find that the thermal solution with the dense ( > $10^7cm^{-3}$) and warm ( ~ 100 K) OH gas reproduces the ratios of detected OH lines. However, our self-consistent PDR 2-D model, which can deal with the IR-pumping effect from the central protostar as well as the warm dust in situ, cannot fit the observational results, suggesting that an irradiated shock model is necessary for a better interpretation.

• Journal of Magnetics
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• 제14권4호
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• pp.137-143
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• 2009

The convergence behavior of the all-electron full-potential linearized augmented plane-wave (FLAPW) method with the explicit orthogonalization (XO) scheme is tested on ferromagnetic bulk body-centered-cubic Fe. Applying a commonly used criterion relating the plane-wave and angular momentum cutoffs, $l_{max}\;=\;R_{MT}K_{max}$, where $R_{MT}$ is the muffin-tin (MT) sphere radius and $K_{max}$ is the plane-wave cutoff for the basis - the total energy is converged and stable for $K_{max}R_{MT}$ = 10. The total energy convergence dependence on the star-function cutoff, $G_{max}$, is minimal and so a $G_{max}$ of 3$K_{max}$ or a large enough $G_{max}$ is a reasonable choice. We demonstrate that the convergence with respect to $l_{max}$ or a fixed large enough $G_{max}\;and\;K_{max}$ are independent, and that $K_{max}$ provides a better measure of the convergence than $R_{MT}K_{max}$. The dependence of the total energy on $R_{MT}$ is shown to be small if the core states are treated equivalently, and that the XO scheme is able to treat systems with significantly smaller $R_{MT}$ than the standard LAPW method. For converged systems, the calculated lattice parameter, bulk modulus, and magnetic moments are in excellent agreement with the experimental values.

• 한국응용과학기술학회지
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• 제33권1호
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• pp.23-29
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• 2016

육방정계 우르자이츠형의 산화아연은 n형 반도체로써 3.37 eV의 넓은 밴드갭 에너지와 60 meV의 큰 엑시톤 바인딩 에너지를 가진 물질이다. 가스센서, 발광 다이오드, 염료 감응 태양 전지, 염료오염의 분해 등의 넓은 범위에서 활용이 가능하다. 합성 시 마이크로파 수열합성법을 사용하게 되면 높은 수율, 빠른 반응속도, 에너지 절약의 장점이 있다. 아민첨가제는 수산이온 생성 및 킬레이트 효과로 인해 산화아연 입자 형상을 조정하는 역할을 한다. 본 논문에서는 전구체로는 질산아연육수화물을 사용하였고, 형상조정제로는 에탄올아민, 에틸렌디아민, 디에틸렌트리아민, 헥사메틸렌테트라민을 사용하였다. 수산화소듐을 사용하여 용액을 pH 11로 조정하였다. 합성된 산화아연은 별모양, 막대형, 꽃모양, 원추형의 다양한 형상을 확인할 수 있었다. 아민첨가제에 의한 물리 화학적 특성과 광학적 특성을 분석하기 위해 XRD, SEM, EDS, FT-IR, UV-vis 스펙트럼, PL 스펙트럼을 사용하였다.

• 한국해양공학회지
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• 제29권6호
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• pp.418-426
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• 2015

Recently, shipping operators have been making efforts to reduce the fuel cost in various ways, such as trim optimization and bulb re-design. Furthermore, IMO restricts the hydro-dioxide emissions to the environment based on the EEDI (Energy Efficiency Design Index), EEOI (Energy Efficiency Operational Indicator), and SEEMP (Ship Energy Efficiency Management Plan). In particular, ship speed is one of the most important factors for calculating the EEDI, which is based on methods suggested by ITTC (International Towing Tank Conference) or ISO (International Standardization Organization). Many shipbuilding companies in Korea have carried out speed trials around the Korea Straits. However, the conditions for these speed trials have not been exactly the same as those for model tests. Therefore, a ship’s speed is corrected by measured environmental data such as the seawater temperature, density, wind, waves, swell, drift, and rudder angle to match the conditions of the model tests. In this study, fundamental research was performed to evaluate the ship resistance performance due to changes in the water temperature and salinity, comparing the ISO method and numerical simulation. A numerical simulation of a KCS (KRISO Container ship) with a free-surface was performed using the commercial software Star-CCM+ under three conditions that were assumed based on the water temperature and salinity data in the Korea Straits. In the simulation results, the resistance increased under low water temperature & high salinity conditions, and it decreased under high water temperature & low salinity conditions. In addition, the ISO method showed the same result as the simulation.

• 천문학논총
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• 제32권1호
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• pp.225-230
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• 2017

The extragalactic background suggests half the energy generated by stars was reprocessed into the infrared (IR) by dust. At z~1.3, 90% of star formation is obscured by dust. To fully understand the cosmic star formation history, it is critical to investigate infrared emission. AKARI has made deep mid-IR observation using its continuous 9-band filters in the NEP field ($5.4deg^2$), using ~10% of the entire pointed observations available throughout its lifetime. However, there remain 11,000 AKARI infrared sources undetected with the previous CFHT/Megacam imaging (r ~25.9ABmag). Redshift and IR luminosity of these sources are unknown. These sources may contribute significantly to the cosmic star-formation rate density (CSFRD). For example, if they all lie at 1< z <2, the CSFRD will be twice as high at the epoch. We are carrying out deep imaging of the NEP field in 5 broad bands (g, r, i, z, and y) using Hyper Suprime-Camera (HSC), which has 1.5 deg field of view in diameter on Subaru 8m telescope. This will provide photometric redshift information, and thereby IR luminosity for the previously-undetected 11,000 faint AKARI IR sources. Combined with AKARI's mid-IR AGN/SF diagnosis, and accurate midIR luminosity measurement, this will allow a complete census of cosmic star-formation/AGN accretion history obscured by dust.

• 천문학회보
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• 제40권1호
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• pp.72.3-72.3
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• 2015

We present the mid-infrared (MIR) luminosity function (LF) of local (z < 0.3) star forming (SF) galaxies based on the AKARI's NEP-Wide Survey data. We utilized a combination of the NEP-Wide point source catalogue containing a large number (114,000) of infrared (IR) sources distributed over the wide (5.4 sq. deg) field and spectroscopic redshift (z) data for 1790 selected targets obtained by optical follow-up surveys with MMT/Hectospec and WIYN/Hydra. The AKARI's continuous $2{\sim}24{\mu}m$ wavelength coverage and the spectroscopic redshifts for sample galaxies enable us to derive accurate spectral energy distributions (SEDs) in the mid-infrared. We carried out SED-fit analysis and employed 1/Vmax method to derive the mid-IR (e.g., $8{\mu}m$, $12{\mu}m$, and $15{\mu}m$ rest-frame) luminosity functions. Our results for local galaxies from the NEP region generally consistent with various previous works for other fields over wide luminosity ranges. The comparison with the results of the NEP-Deep data implies the luminosity evolution from higher redshifts towards the present epoch. We attempted to fit our derived LFs to the double power-laws and present the resulting power indices. We also examined the correlation between mid-IR luminosity and total IR luminosity.