• 대기
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• 제21권2호
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• pp.131-142
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• 2011

Spectral solar irradiances were observed using a visible and UV Multi-Filter Rotating Shadowband Radiometer on the rooftop of the Science Building at Yonsei University, Seoul ($37.57^{\circ}N$, $126.98^{\circ}E$, 86 m) during one year period in 2006. 1-min measurements of global(total) and diffuse solar irradiances over the solar zenith angle (SZA) ranges from $20^{\circ}$ to $70^{\circ}$ were used to examine the effects of clouds and total optical depth (TOD) on enhancing four solar irradiance components (broadband 395-955 nm, UV channel 304.5 nm, visible channel 495.2 nm, and infrared channel 869.2 nm) together with the sky camera images for the assessment of cloud conditions at the time of each measurement. The obtained clear-sky irradiance measurements were used for empirical model of clear-sky irradiance with the cosine of the solar zenith angle (SZA) as an independent variable. These developed models produce continuous estimates of global and diffuse solar irradiances for clear sky. Then, the clear-sky irradiances are used to estimate the effects of clouds and TOD on the enhancement of surface solar irradiance as a difference between the measured and the estimated clear-sky values. It was found that the enhancements occur at TODs less than 1.0 (i.e. transmissivity greater than 37%) when solar disk was not obscured or obscured by optically thin clouds. Although the TOD is less than 1.0, the probability of the occurrence for the enhancements shows 50~65% depending on four different solar radiation components with the low UV irradiance. The cumulus types such as stratoculmus and altoculumus were found to produce localized enhancement of broadband global solar irradiance of up to 36.0% at TOD of 0.43 under overcast skies (cloud cover 90%) when direct solar beam was unobstructed through the broken clouds. However, those same type clouds were found to attenuate up to 80% of the incoming global solar irradiance at TOD of about 7.0. The maximum global UV enhancement was only 3.8% which is much lower than those of other three solar components because of the light scattering efficiency of cloud drops. It was shown that the most of the enhancements occurred under cloud cover from 40 to 90%. The broadband global enhancement greater than 20% occurred for SZAs ranging from 28 to $62^{\circ}$. The broadband diffuse irradiance has been increased up to 467.8% (TOD 0.34) by clouds. In the case of channel 869.0 nm, the maximum diffuse enhancement was 609.5%. Thus, it is required to measure irradiance for various cloud conditions in order to obtain climatological values, to trace the differences among cloud types, and to eventually estimate the influence on solar irradiance by cloud characteristics.

• 대한원격탐사학회지
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• 제22권6호
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• pp.507-518
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• 2006

지표면에서 방출된 $11{\mu}m$와 $12{\mu}m$의 복사량은 대기 입자에 의해 선택적으로 산란되고 흡수된다. 에어로솔이 대기 중에 존재할 경우 지표면에서 방출되는 $11{\mu}m$의 복사량이 $12{\mu}m$보다 흡수를 많이 하므로 밝기 온도가 낮게 나타나고, 반대로 구름에 대해서는 $12{\mu}m$가 흡수를 많이 하여 $11{\mu}m$의 밝기 온도가 높게 나타난다. 그러므로 $11{\mu}m$와 $12{\mu}m$의 밝기 온도 차이(BTD)를 통해 구름과 에어로솔의 존재 유무를 판별할 수 있고, 에어로솔의 광학 두께를 추정할 수 있다. 본 연구에서는 대기의 구성 물질과 연직 분포 상태, 지표면의 온도와 형태, 그리고 에어로솔의 구성성분에 따라 BTD 경계값과 민감도를 분석하였다. BTD 경계값은 이론적으로 $0^{\circ}K$라고 알려져 있으나 본 연구에서 US 표준 대기 상태일 때 $0.8^{\circ}K$의 경계값을 보인다. BTD 값은 태양 천정각, 에어로솔의 고도, 지표면 반사도, 그리고 대기의 연직적 온도 분포에 따라서는 영향을 적게 받았다. 그러나 위성 천정각, 지표면 온도와 방출율, 연직적 수증기 분포에 대해 영향이 크게 나타나며 에어로솔 탐지에 50%이상의 오차를 유발할 수도 있다. 그러므로 BTD 방법을 사용하는데 있어 주의가 요구되며, BTD값에 영향을 미치는 인자를 보정해 준다면 좀 더 정확한 에어로솔 탐지가 가능하리라 사료된다.

• 대한원격탐사학회지
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• 제34권6_3호
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• pp.1369-1382
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• 2018

국내 외 다중분광 위성의 수가 증가하고 자료를 획득할 수 있는 경로가 넓어짐에 따라 원하는 시기의 영상 취득 및 활용이 가능할 것으로 기대된다. 하지만 다른 촬영시간, 주기 및 공간해상도를 가지기 때문에 자료의 불일치 문제가 존재한다. 특히, 밴드대역폭 차이는 동일한 시기에 촬영된 영상일지라도 서로 다른 반사도를 산출하며, 식생지수와 같은 식생 활력도 분석에 있어 큰 불확실성이 발생한다. 본 연구는 KOMPSAT-3의 농업분야 활용을 위해 타 다중분광위성과의 밴드대역폭 차이에 따른 Spectral Band Adjustment Factor(SBAF)를 산정하고 실제 적용을 통해 융합 활용 가능성을 평가하였다. 사막지역에서 취득된 초분광 위성영상을 활용하여 SBAF를 산정하였고, 작물 주산지 지역에 SBAF를 적용한 결과 식생지수는 천정각이 24도로 촬영된 합천지역을 제외한 다른 지역에서 상대백분율 차이가 3% 이내로 높은 일치율을 보였다. SBAF 산정을 위해 본 연구는 한 세트의 영상을 활용하였고 이는 SBAF의 계절 및 태양 천정각에 따른 변화를 고려하지 않아 불확실성이 높을 것으로 판단되며, 향후 이러한 문제를 해결하기 위해 장기간 분석이 필요할 것으로 판단된다.

• 대한원격탐사학회지
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• 제35권3호
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• pp.483-489
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• 2019

True color 영상은 자연색과 유사한 색상이 표출되며 이는 복잡한 지구의 대기 현상 및 지표의 변화에 빠른 모니터링이 가능하다는 장점이 있다. 현재 다양한 기관에서 true color 영상을 생산 중이며 우리나라에서도 차세대 기상위성으로 세대교체가 이루어져 true color 영상 생산의 필요성이 대두되고 있다. 따라서 본 연구에서는 Himawari-8 위성에 탑재된 Advanced Himawari Imager(AHI) 센서의 Top of Atmosphere(TOA) 자료를 이용해 true color 영상 생산을 위한 시각화 향상을 수행하였다. 시각화 향상을 위해 본 연구는 Nonlinear enhancement과 Histogram equalization 두 가지 기법을 각각 수행하였다. 이를 비교해 본 결과, Histogram equalization는 Nonlinear enhancement 대비 Solar Zenith Angle(SZA) $70^{\circ}$ 이상 지역과 해양 영역에서 청색 계열이 강한 영상이 나타났으며, Nonlinear enhancement 기법의 경우 Histogram equalization 기법과 비교했을 때 식생 영역이 붉은 특징이 나타났다.

• 대기
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• 제23권2호
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• pp.123-130
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• 2013

Despite the extensive investigations to understand the difference between ground-based and space-borne measurements, there still exist differences in total ozone (TO) measured at those two different platforms. Comparisons were carried out for the first time between TO data obtaiend from the ground based Dobson and Brewer spectrophotometers, and the Ozone Monitoring Instrument (OMI) on board EOS-Aura satellite in a megacity site in Northeast Asia. The TO values retrieved by the OMI-DOAS (Differential optical absorption spectroscopy) algorithm tend to be lower than those measured by the ground based sensors in spring and summer as well as the low solar zenith angle condition. We found that such underestimation of the OMI-DOAS TO is caused by tropospheric ozone underestimated by the OMI-DOAS algorithm when tropospheric ozone are significantly enhanced.

• 천문학회지
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• 제34권1호
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• pp.25-29
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• 2001

We have constructed a non-spherical model for the hot oxygen corona of Mars by including the effects of planetary rotation and diurnal variation of the Martian ionosphere. Exospheric oxygen densities are calculated by integrating ensemble of ballistic and escaping oxygen atoms from the exobase over the entire planet. The hot oxygen atoms are produced by dissociative recombination of $O^+_2$, the major ion in the Martian ionosphere. The densities of hot oxygen atoms at the exobase are estimated from electron densities which have been measured to vary with solar zenith angle. Our model shows that the density difference of hot oxygen atoms between noon and terminator is about two orders of magnitude near the exobase, but reduces abruptly around altitudes of 2000 km due to lateral transport. The diurnal variation of hot oxygen densities remains significant up to the altitude of 10000 km. The diurnal variation of the hot oxygen corona should thus be considered when the upcoming Nozomi measurements are analyzed. The non-spherical model of the hot oxy-gen corona may contribute to building sophisticate solar wind interaction models and thus result in more accurate escaping rate of oxygens from Mars.

• 천문학회보
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• 제35권2호
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• pp.58.1-58.1
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• 2010

Telescope Array (TA) experiment in Utah, USA, observes ultrahigh-energy cosmic rays (UHECRs); UHECRs refer cosmic rays with energy above $10^{18}eV$. Using COSMOS and CORSIKA, we have produced a library of over 1000 thinned extensive air shower (EAS) simulations with the primary energies ranging from $10^{18.5}eV$ to $10^{20.25}eV$ and the zenith angle of primary cosmic ray particle from $0^{\circ}$ to $45^{\circ}$. Here, we present the energy spectrum of particles arriving at the ground. We have also calculated the detector response evaluated using GEANT4 simulations. Here, we discuss S(800), i.e. the signal at a distance of 800 m from the shower core, as the primary energy estimator.

• 대한원격탐사학회:학술대회논문집
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• 대한원격탐사학회 2007년도 Proceedings of ISRS 2007
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• pp.149-152
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• 2007

The detection of yellow sand dust using satellite has been utilized from various bands from ultraviolet to infrared channels. Among them, Infrared channels have an advantage of detecting aerosols over high reflecting surface as well as during nighttime. Especially, brightness temperature difference between 11 and 12{\mu}m(BTD) was often used to distinguish between water cloud and yellow sand, because Ice and liquid water particles preferentially absorb longer wavelengths while aerosol particles preferentially absorb shorter wavelengths. We have found that the BTD significantly depends on surface temperature, emissivity, and zenith angle and thereby the threshold of BTD. In order to overcome these problems, we have constructed the background brightness temperature threshold of BTD and then subtracted it from BTD. Along with this, we utilized high temporal coverage of geostationary satellite, MTSAT-1R, to verify the reliability of the retrieved signal in conjunction with forecasted wind information. The statistical score test illustrated that this newly developed algorithm showed a promising result for detecting mineral dust by reducing the errors in the current BTD method.

• 천문학회보
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• 제36권2호
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• pp.128.2-128.2
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• 2011

Experiments to study high-energy cosmic rays (CRs) employ Monte Carlo codes for extensive air shower (EAS) simulations to figure out the properties of CRs. COSMOS and CORSIKA among EAS simulation codes are currently being used to analyze the data of the Telescope Array experiment. We have generated a library of about 10,000 simulated EASs with the primary energy ranging from $10^{18.5}eV$ to $10^{20}eV$ and the zenith angle of primary particles ranging from 0 to 45 degree for proton and iron primaries. We have compared the results predicted by CORSIKA and COSMOS under the same condition. In this talk, we show the differences in the energy spectra at the ground, the longitudinal shower profile as a function of atmospheric depth, the Calorimetric energy, and the Xmax distribution. We also discuss the lateral distribution function obtained from GEANT4 simulations which is being used to measure the detector response.

• 한국태양에너지학회 논문집
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• 제36권3호
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• pp.33-43
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• 2016

Daylight is an important factor which influences building energy efficiency and visual comfort for occupants. It is important to predict precise sky luminance at the early stages of design to reduce light energy in the building. This study predicted sky luminance distributions of standard sky model(CIE overcast sky, CIE clear sky) that was provided from the CIE(Commission internationale de $l^{\prime}{\acute{e}}clairage$). Afterward, result of sky luminance was compared and verified with simulation value of Radiance program. From the CIE overcast sky, zenith and horizon ratio is about 3:1. From the CIE clear sky, luminance value gets most high value around the sun. On the other hand, luminance value is the lowest in the opposite direction of the sun when angle is $90^{\circ}$ between the sun and sky element. As a result of comparing the calculation results with Radiance program, sky luminance prediction error rate is 0.4~1.3% when it is CIE overcast sky. Also, sky luminance prediction error rate is 0.3~1.5% when it is CIE clear sky. When compared with the results of radiance simulation, it was evaluated as fairly accurate.