• 대한전자공학회:학술대회논문집
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• 대한전자공학회 2001년도 The 6th International Symposium of East Asian Resources Recycling Technology
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• pp.331-336
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• 2001

Aragonite type of precipitated calcium carbonate was synthesized by the successive reaction with hybridization of waste scallop shells with limestone. In the first step, carbonation was performed by using calcined limestone with low brightness, followed by the additional carbonation using calcined-hydrous scallop shells with high brightness. The temperature and the amount ratio of calcined limestone to calcined-hydrous scallop shells were examined as parameters in the experimental conditions. The products were characterized by XRD, SEM. in addition to measurements of brightness index. the specific surface area, and bulk density. The amount ratio of limestone to scallop shell affected not only the brightness but also morphologies of products. The increase in relative amounts of limestone leads to decrease in brightness and bumpy surface of particles. High temperature reaction produces aragonite particles with longer sizes and higher bulk densities. This study has made an attempt to establish the synthesis of aragonite with high brightness and high strength by utilization of waste scallop shells.

• 대한원격탐사학회:학술대회논문집
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• 대한원격탐사학회 2007년도 Proceedings of ISRS 2007
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• pp.282-285
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• 2007

Satellite observed brightness temperature simulation using a radiative transfer model (here after, RTM) is useful for various fields, for example sensor design and channel selection by using theoretically calculated radiance data, development of satellite data processing algorithm and algorithm parameter determination before launch. This study is focused on elaborating the simulation procedure, and analyzing of difference between observed and modelled clear sky brightness temperatures. For the CMDPS (COMS Meteorological Data Processing System) development, the simulated clear sky brightness temperatures are used to determine whether the corresponding pixels are cloud-contaminated in cloud mask algorithm as a reference data. Also it provides important information for calibrating satellite observed radiances. Meanwhile, simulated brightness temperatures of COMS channels plan to be used for assessing the CMDPS performance test. For these applications, the RTM requires fast calculation and high accuracy. The simulated clear sky brightness temperatures are compared with those of MTSAT-1R observation to assess the model performance and the quality of the observation. The results show that there is good agreement in the ocean mostly, while in the land disagreement is partially found due to surface characteristics such as land surface temperature, surface vegetation, terrain effect, and so on.

• 스마트미디어저널
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• 제6권3호
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• pp.57-63
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• 2017

차량번호인식 개선을 위해서는 무엇보다 양질의 차량이미지를 획득하는 것이 무엇보다 먼저 선행되어야 하는 필수적인 요소이다. 일반적인 도로영상들은 시간, 햇빛, 날씨 등 다양한 환경의 영향을 받아 번호판 밝기가 일률적이지 않고 다양한 형태로 나타나기 때문에 여러 가지 이미지 보정 기능을 거치게 되고 이로 인하여 인식속도 저하, 인식률 저하 등이 나타난다. 따라서, 본 논문에서는 실시간 영상 촬영 시 번호판 주위의 밝기를 측정하여 카메라의 shutter, bright, gain등 이미지 밝기와 품질에 영향을 주는 각 요소를 실시간으로 제어하여 빠르고 선명한 고품질의 차량 이미지 촬영하기 위해 실시간 도로 영상을 통하여 제안된 방법을 테스트 하였다.

• 한국멀티미디어학회논문지
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• 제19권9호
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• pp.1723-1737
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• 2016

When watching 3D contents, people often experience various visual discomforts like tiredness, dryness, headaches, and dizziness. Previous researches on visual discomfort analyzed and concluded vergence-accommodation conflict, viewing distance, and brightness changes to be the causes of visual discomfort. Yet it is necessary to systematically analyze the visual discomfort due to the changes in object, background brightness and viewing distance. In this paper, we produce four videos that have four different background brightness and two different viewing distances to solve analyze the visual discomfort from watching 3D contents. We measure and analyze eye-blink and saccadic movement, saccadic latency, Nearest Point of Convergence (NPC), and participant survey for amore accurate result compared to previous researches. Our results show that the eye-blink rate and saccadic latency increase when the background is bright and viewing distance is close while the saccadic movement decreases in the same environment. However, NPC only changes when the background brightness changes. We confirm that the bright background and near viewing distance create greater visual discomfort and decrease depth perception abilities.

• 방송공학회논문지
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• 제19권4호
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• pp.453-467
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• 2014

일반적인 히스토그램 평활화는 화질향상을 위한 명암대비 향상 효과가 뛰어나다. 하지만 과도한 밝기 값의 변화가 나타나기 때문에 영상의 평균밝기가 프레임 단위로 변화하는 TV와 같은 동영상 응용분야에 적용하기에는 부적합하다. 이러한 단점을 해결하기 위하여 히스토그램 평활화의 변형된 방법에 대한 다양한 연구가 이루어져 왔다. 그러나 기존의 방법들은 과포화현상(over-enhancement), 계조 현상(false-contouring)과 같은 화질 열화를 보인다. 본 논문에서는 차별적 히스토그램 압축방법을 기반으로 하는 목표 평균 밝기값을 이용한 분할 히스토그램 평활화를 통해서 개선된 명암대비 향상 기법을 제안한다. 제안한 방법은 평균 밝기값을 기준으로 히스토그램을 분할하고, 각 영역에 대해 히스토그램을 빈도수에 따라 차별적으로 압축한다. 그리고 변형된 히스토그램을 목표 평균 밝기값 기준으로 평활화한다. 이를 통하여 화질 열화를 억제하고, 동영상의 각 프레임의 평균밝기 변화를 유지하면서 명암대비를 개선시킨다. 실험 결과 제안방법은 기존 방법에 비해 동영상에서 각 프레임의 평균밝기를 잘 유지하고, 화질 열화 없이 좋은 명암대비 향상 효과를 보였다.

• 지적과 국토정보
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• 제47권2호
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• pp.19-37
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• 2017

VIIRS-DNB 데이터는 기존의 DMSP-OLS 데이터에 비해 야간에 발생하는 빛의 밝기를 측정하는데 더 우수한 성능을 보여준다. 하지만 지금까지 우리나라에서 VIIRS-DNB 데이터를 이용해 야간 빛의 분포 변화를 분석한 연구는 상당히 드물다. 이 연구에서는 우리나라의 수도권을 대상으로 2013~2016년간의 야간 빛의 분포 및 변화 패턴을 파악하고, 공간회귀모델을 통해 그 요인을 분석하였다. 이를 위해 두 시점 간의 변화를 살펴봄은 물론 계절간 변화 양상 또한 함께 분석하였다. 주요한 결과는 다음과 같다. 첫째, 2013년과 2016년 두 시점 모두 야간 빛은 서울과, 인천, 그리고 서울과 인접한 경기도의 도시에 집중되어 인구밀도 및 주거지관련요인, 경제토지이용관련요인 등과의 연관성을 나타내었다. 둘째, 2013년과 2016년을 비교해보면 야간 빛의 강도는 특히 서울에서 약화되는 경향을 보이고 있는데, 이는 인구밀도의 변화 및 산업용 건물의 비중과 관련된 것으로 나타났다. 셋째, 서울, 그리고 인천과 경기도의 주변 지역들은 야간 빛의 계절 변동성이 높게 나타났는데, 겨울(12월, 1월, 2월) 및 가을(10월, 11월)에 빛의 강도가 가장 강하게 나타났다. 넷째, 야간 빛의 계절간 변동은 적설면적 변화와 유의미하게 양적 상관관계 나타났고, 알베도의 변화와 유의미하게 음적 상관관계 나타났다.

• 만화애니메이션 연구
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• 통권15호
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• pp.73-88
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• 2009

이 논문에서는 시각적으로 명암이 인간의 정서에 영향을 미친다는 그레이브스의 명암이론을 적용하여 "라이온 킹" 에서 사용된 명암의 유형을 분석하고 작품 내에서 시각적으로 표현된 명암이 내러티브에서 전개되는 정서의 흐름과 어떠한 관계를 맺고 있는지에 대한 유형을 분석하였다. 이를 통하여 명암이 시각이미지에 끼치는 영향과 더불어 정서적인 분위기 표현에 중요한 요소로 작용한다는 점을 규명하고자 하였다. 애니메이션에서는 실사 영화와는 달리 내러티브상에서 전개되는 캐릭터들의 정서적 변화에 따른 이미지 연출이 더욱 강조 된다. 이는 관객들의 감정이입을 강화시키는 중요한 수단이 된다.

• 한국안전학회지
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• 제27권4호
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• pp.13-19
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• 2012

The purpose of this study is to extract the major factors related to the deterioration mechanism of white organic light-emitting diodes(WOLED) by performing accelerated testing of temperature, voltage, time, etc., and to develop an accelerated life test(ALT) model. The measurement results of the brightness of the WOLED exhibited that their average brightness tended to increase as the operating voltage increased and that the half-life period of the brightness appeared after approximately 400 hours when the operating voltage was 20V and the ambient temperature was $85^{\circ}C$. It could be seen that although the WOLED showed comparatively the same brightness when the initial acceleration began after the operating voltage was applied to it, its brightness changed excessively after the WOLED's thermal storage had been made. In addition, it was observed that the half-life period was reduced as the ambient temperature and applied voltage increased. The strength of the WOLED which had been maintained in the range of visible light at the maximum load was reduced by the deterioration of the organic light emitting material due to the influence of the operating voltage and temperature, and the reduction of emitted light was small at low voltage and temperature. It could be seen that the failure of the WOLED during the ALT was caused by wear due to load accumulation over time, and that Weibull distribution was appropriate for the life distribution and acceleration was established between test conditions. From the WOLED analysis, it is thought that factors influencing the brightness deterioration are voltage, temperature, etc., and that comprehensive analysis considering discharge control, dielectric tangent margin, etc., would further increase the reliability.

• 한국인쇄학회지
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• 제29권3호
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• pp.105-124
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• 2011

TFT-LCD consists of LCD panel on the top, circuit unit on the side and BLU on the bottom. The recent development issues of BLU-dependent TFT-LCD have been power consumption minimization, slimmerization and size maximization. As a result of this trend, LED is adopted as BLU instead of CCFL to increase brightness and to reduce thickness. In liquid crystal displays, the light efficiency is below 10% due to the loss of light in the path from a light source to an LCD panel and presence of absorptive polarizer. This low efficiency results in low brightness and high power consumption. One way to circumvent this situation is to use a reflective polarizer between backlight units and LCD panels. Since a nano-wire grid polarizer has been known as a reflective polarizer, an idea was proposed that it can be used for the enhancement of the brightness of LCD. The use of reflective polarizing film is increasing as edge type LED TV and 3D TV markets are growing. This study has been carried out to fabrication of the nano-wire grid polarizer(NWGP) and investigated the brightness enhancement of LCD through polarization recycling by placing a NWGP between an c and a backlight unit. NWGPs with a pitch of 200nm were fabricated using laser interference lithography and aluminum sputtering and wet etching. And The NWGP fabrication process was using by the UV imprinting and was applied to plastic PET film. In this case, the brightness of an LCD with NWGPs was 1.21 times higher than that without NWGPs due to polarization recycling.

• 천문학회보
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• 제36권2호
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• pp.117.1-117.1
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• 2011

We present the smoothness of mid-infrared sky brightness from the Japanese infrared astronomical satellite, AKARI observations. AKARI monitored the north ecliptic pole (NEP) during its cold phase with nine wavebands from 2.4 to 24 ${\mu}m$, out of which six mid-infrared bands are used in this study. Simple sinusoidal fit to the seasonal variation of the sky brightness shows that the mid-infrared brightness towards the NEP is not affected by small-scale features of the interplanetary dust cloud. We applied the power spectrum analysis to the images to search for the fluctuation of sky brightness. The fluctuation powers at 200 arcsecond are estimated to be at most $1.58{\pm}0.33\;nW\;m^{-2}sr^{-1}$ or 0.13% of the total brightness at $7{\mu}m$ and a tleast $0.64{\pm}0.11\;nW\;m^{-2}sr^{-1}$ or 0.02% at $18{\mu}m$. The residual fluctuations at a few arcminute scales at short mid-infrared wavelengths (7, 9, and 11 ${\mu}m$) are consistent with those expected from the diffuse galactic light. At long mid-infrared wavelengths (15, 18, and 24 ${\mu}m$) the measured fluctuations are comparable to or smaller than the one caused by photon noise and their sources are not identified. We conclude that the upper limit of the fluctuation in the zodiacal light is about 0.02% of the sky brightness.