• 항공우주기술
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• 제12권1호
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• pp.152-162
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• 2013

달의 방사조도는 위성 가시채널 검출기의 성능을 감시하기 위해서 사용된다. 본 논문에서는 천리안위성 FDS (Flight Dynamics Subsystem)에서 생성한 태양, 달, 위성의 위치 정보를 이용하여 달의 방사조도를 계산하는 방법 및 결과를 설명한다. 계산 결과는 천리안위성 기상탑재체 가시채널 검출기의 성능저하를 검출하고 보상하기 위한 알고리즘에 적용되었다.

• 대한치과보존학회:학술대회논문집
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• 대한치과보존학회 2008년도 Spring Scientific Meeting(the 129th) of Korean Academy if Conservative Dentistry
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• pp.213-223
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• 2008

광물리학적 특성 분석을 위해 Apollo 95E (DMT Systems, Orange, CA : PAC 광중합기), Elipar Freelight 2 (3M ESPE, MN, USA; LED 광중합기) 그리고 VIP Junior (Bisco, Schaumberg, IL, USA : QTH 광중합기), 3종의 광중합기의 총광강도(Total intensity)와 spectral distribution을 측정하였고 특정 파장에 해당되는 광강도(Energy density)를 분석하였다. 상아질 전단접착강도의 측정을 위해 Scotchbond Multipurpose (3M ESPE), Single bond (3M ESPE) 그리고 Clearfil SE bond (Kuraray)가 사용되었다. Plasma Arc Curing light (Apollo 95E) 광중합기는 여러개의 최대정점을 가지며 넓은 spectral distribution과 $2307mW/cm^2$의 높은 광강도를 나타내었고, VIP Junior 광중합기는 490 nm에서 최대정점을 갖는 넓은 spectral distribution을 나타내었고, Elipar Freeelight 2 광중합기는 462 nm의 최대정점 주위로 좁은 spectral distribution을 보였다. Two-Way ANOVA와 Bonferroni's multiple comparison test를 이용하여 상아질 전단접착강도를 분석한 결과, PAC 광중합기와 LED 광중합기 간에 유의성 있는 차이를 보이지 않았으며 (P > 0.05), 상아질 접착제와 광중합기의 교호관계에도 유의성이 없었다. 그러나 상아질 접착제는 상호간에 유의성 있는 차이를 보였다 (P < 0.00).

• Restorative Dentistry and Endodontics
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• 제33권3호
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• pp.213-223
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• 2008

광물리학적 특성 분석을 위해 Apollo 95E (DMT Systems, Orange, CA; PAC 광중합기), Elipar Freelight 2 (3M ESPE, MN, USA; LED 광중합기) 그리고 VIP Junior (Bisco, Schaumberg, IL, USA; QTH 광중합기), 3종의 광중합기의 총광강도(Total intensity)와 spectral distribution을 측정하였고 특정 파장에 해당되는 광강도 (Energy density)를 분석하였다. 상아질 전단접착강도의 측정을 위해 Scotchbond Multipurpose (3M ESPE), Single bond (3M ESPE) 그리고 Clearfil SE bond (Kuraray)가 사용되었다. Plasma Arc Curing light (Apollo 95E) 광중합기는 여러개의 최대정점을 가지며 넓은 spectral distribution과 $2307mw/cm^2$의 높은 광강도를 나타내었고, VIP Junior 광중합기는 490nm에서 최대정점을 갖는 넓은 spectral distribution을 나타내었고, Elipar Freeelight 2 광중합기는 462 nm의 최대정점 주위로 좁은 spectral distribution을 보였다. Two-Way ANOVA와 Bonferroni's multiple comparison test를 이용하여 상아질 전단접착강도를 분석한 결과, PAC 광중합기와 LED 광중합기 간에 유의성 있는 차이를 보이지 않았으며 (P > 0.05), 상아질 접착제와 광중합기의 교호관계에도 유의성이 없었다. 그러나 상아질 접착제는 상호간에 유의성 있는 차이를 보였다 (P < 0.001).

• 대한원격탐사학회:학술대회논문집
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• 대한원격탐사학회 2007년도 Proceedings of ISRS 2007
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• pp.156-158
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• 2007

The radiance observed from the ocean depends on the illumination and viewing geometry along with the water properties, and this variation is called the bidirectional effect which is important to be considered in ocean color remote sensing. In the present study, as a preliminary step, the spectral-angular radiances in coastal water were investigated with experiments for a range of viewing geometric conditions $(0-70^{\circ})$. Over a phytoplankton-dominated water surface the upward radiance for visible and near-infrared wavelengths (example, SeaWiFS and GOCI) increased at nadir and decreased toward the near-horizon, becoming dependent of viewing angles (with higher radiance at nadir view angle and lower radiance at near-horizon viewing angle). This variations were better expressed by the Q-factor, which relates upwelling radiance to the upwelling irradiance (i.e., $Q=E_u/L_u$, also dependent on Sun's position). The Q-factor for this case was more non-uniform with the considered wavelengths and was dependent on viewing geometric conditions. These experimental results confirm the previous similar findings in other coastal waters.

• Journal of Astronomy and Space Sciences
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• 제21권4호
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• pp.329-342
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• 2004

In this paper, we present preliminary feasibility studies on three types of solar observation payloads for future Korean Science and Technology Satellite (STSAT) programs. The three candidates are (1) an UV imaging telescope, (2) an UV spectrograph, and (3) an X-ray spectrometer. In the case of UV imaging telescope, the most important constraint seems to be the control stability of a satellite in order to obtain a reasonably good spatial resolution. Considering that the current pointing stability estimated from the data of the Far ultraviolet Imaging Spectrograph (FIMS) onboard the Korean STSAT-1, is around 1 arc minutes/sec, we think that it is hard to obtain a spatial resolution sufficient for scientific research by such an UV Imaging Telescope. For solar imaging missions, we realize that an image stabilization system, which is composed of a small guide telescope with limb sensor and a servo controller of secondary mirror, is quite essential for a very good pointing stability of about 0.1 arcsec. An UV spectrograph covering the solar full disk seems to be a good choice in that there is no risk due to poor pointing stability as well as that it can provide us with valuable UV spectral irradiance data valuable for studying their effects on the Earth's atmosphere and satellites. The heritage of the FIMS can be a great advantage of developing the UV spectrograph. Its main disadvantage is that two major missions are in operation or scheduled. Our preliminary investigations show that an X-ray spectrometer for the full disk Sun seems to be the best choice among the three candidates. The reasons are : (1) high temporal and spectral X-ray data are very essential for studying the acceleration process of energetic particles associated with solar flares, (2) we have a good heritage of X-ray detectors including a rocket-borne X-ray detector, (3) in the case of developing countries such as India and Czech, solar X-ray spectrometers were selected as their early stage satellite missions due to their poor pointing stabilities, and (4) there is no planned major mission after currently operating Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) mission. Finally, we present a preliminary design of a solar X-ray spectrometer covering soft X-ray (2 keV) to gamma ray (10 MeV).