• 한국전기전자재료학회논문지
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• 제36권1호
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• pp.49-55
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• 2023

The deposition of indium zinc oxide (IZO) thin films was carried out on substrate at room temperature by RF magnetron sputtering. The effects of substrate temperature, RF power and deposition pressure were investigated with respect to physical and optical properties of films such as deposition rate, electrical properties, structure, and transmittance. As the RF power increases, the resistivity gradually decreases, and the transmittance slightly decreases. For the variation of deposition pressure, the resistivity greatly increases, and the transmittance is decreased with increasing deposition pressure. As a result, it was demonstrated that an IZO film with the resistivity of 3.89 × 10^-4 Ω∙cm, the hole mobility of 51.28 cm²/Vs, and the light transmittance of 86.89% in the visible spectrum at room temperature can be prepared without post-deposition annealing.

• 한국신재생에너지학회:학술대회논문집
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• 한국신재생에너지학회 2010년도 추계학술대회 초록집
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• pp.39.2-39.2
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• 2010

In this work we have investigated electrical and optical properties of interface for ITO/Si with shallow doped emitter. The ITO is prepared by DC magnetron sputter on p-type monocrystalline silicon substrate. As an experimental result, The transmittance at 640nm spectra is obtained an average transmittance over 85% in the visible range of the optical spectrum. The energy bandgap of ITO at oxygen flow from 0% to 4% obtained between 3.57eV and 3.68eV (ITO : 3.75eV). The energy bandgap of ITO is depending on the thickness, sturcture and doping concentration. Because the bandgap and position of absorption edge for degenerated semiconductor oxide are determined by two competing mechanism; i) bandgap narrowing due to electron-electron and electron-impurity effects on the valance and conduction bands (> 3.38eV), ii) bandgap widening by the Burstein-Moss effect, a blocking of the lowest states of the conduction band by excess electrons( < 4.15eV). The resistivity of ITO layer obtained about $6{\times}10^{-4}{\Omega}cm$ at 4% of oxygen flow. In case of decrease resistivity of ITO, the carrier concentration and carrier mobility of ITO film will be increased. The contact resistance of ITO/Si with shallow doped emitter was measured by the transmission line method(TLM). As an experimental result, the contact resistance was obtained $0.0705{\Omega}cm^2$ at 2% oxygen flow. It is formed ohmic-contact of interface ITO/Si substrate. The emitter series resistance of ITO/Si with shallow doped emitter was obtained $0.1821{\Omega}cm^2$. Therefore, As an PC1D simulation result, the fill factor of EWT solar cell obtained above 80%. The details will be presented in conference.

• 천문학회보
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• 제38권2호
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• pp.89.1-89.1
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• 2013

We present a multiwavelength study of the X-class flare, which occurred in active region (AR) NOAA 11339 on 3 November 2011. The EUV images recorded by SDO/AIA show the activation of a remote filament (located north of the AR) with footpoint brightenings about 50 min prior to the flare occurrence. The kinked filament rises-up slowly and after reaching a projected height of ~49 Mm, it bends and falls freely near the AR, where the X-class flare was triggered. Dynamic radio spectrum from the Green Bank Solar Radio Burst Spectrometer (GBSRBS) shows simultaneous detection of both positive and negative drifting pulsating structures (DPSs) in the decimetric radio frequencies (500-1200 MHz) during the impulsive phase of the flare. The global negative DPSs in solar flares are generally interpreted as a signature of electron acceleration related to the upward moving plasmoids in the solar corona. The EUV images from AIA $94{\AA}$ reveal the ejection of multiple plasmoids, which move simultaneously upward and downward in the corona during the magnetic reconnection. The estimated speeds of the upward and downward moving plasmoids are ~152-362 and ~83-254 km/s, respectively. These observations strongly support the recent numerical simulations of the formation and interaction of multiple plasmoids due to tearing of the current-sheet structure. On the basis of our analysis, we suggest that the simultaneous detection of both the negative and positive DPSs is most likely generated by the interaction/coalescence of the multiple plasmoids moving upward and downward along the current-sheet structure during the magnetic reconnection process. Moreover, the differential emission measure (DEM) analysis of the active region reveals presence of a hot flux-rope structure (visible in AIA 131 and $94{\AA}$) prior to the flare initiation and ejection of the multi-temperature plasmoids during the flare impulsive phase.

• Journal of Astronomy and Space Sciences
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• 제29권4호
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• pp.329-336
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• 2012

Korea Astronomy and Space Science Institute researchers have installed and operated magnetometers at Bohyunsan Observatory to measure the Earth's magnetic field variations in South Korea. In 2007, we installed a fluxgate magnetometer (RFP-523C) to measure H, D, and Z components of the geomagnetic field. In addition, in 2009, we installed a Overhauser proton sensor to measure the absolute total magnetic field F and a three-axis magneto-impedance sensor for spectrum analysis. Currently three types of magnetometer data have been accumulated. In this paper, we use the H, D, Z components of fluxgate magnetometer data to investigate the characteristics of mid-latitude geomagnetic field variation. To remove the temporary changes in Earth's geomagnetic filed by space weather, we use the international quiet days' data only. In other words, we performed a superposed epoch analysis using five days per each month during 2008-2011. We find that daily variations of H, D, and Z shows similar tendency compared to previous results using all days. That is, H, D, Z all three components' quiet intervals terminate near the sunrise and shows maximum 2-3 hours after the culmination and the quiet interval start from near the sunset. Seasonal variations show similar dependences to the Sun. As it becomes hot season, the geomagnetic field variation's amplitude becomes large and the quiet interval becomes shortened. It is well-known that these variations are effects of Sq current system in the Earth's atmosphere. We confirm that the typical mid-latitude geomagnetic field variations due to the Sq current system by excluding all possible association with the space weather.

• 한국진공학회:학술대회논문집
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• 한국진공학회 2009년도 제38회 동계학술대회 초록집
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• pp.149-149
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• 2010

The double-layer antireflection (DLAR) coatings have significant advantages over single-layer antireflection (SLAR) coatings. This is because they will be able to cover a broad range of the solar spectrum which would enhance the overall performance of solar cells. Moreover films deposited at high frequency are expected to show excellent and UV-stable passivation in the refractive index that we adopted. In this work, we present a novel DLAR coating using SiNx:H thin films with refractive indices 1.9 and 2.3 as the top and bottom layers. This approach is cost effective when compared to earlier DLAR coatings with two different materials. SiNx:H films were deposited by Plasma enhanced chemical vapor deposition (PECVD) technique using $SiH_4$, $NH_3$ and $N_2$ gases with flow rates 20~80sccm, 200sccm and 85 sccm respectively. The RF power, plasma frequency and substrate temperature for the deposition were 300W, 13.56 MHz and $450^{\circ}C$, respectively. The optimum thickness and refractive indices values for DLAR coatings were estimated theoretically using Macleod simulation software as 82.24 nm for 1.9 and 68.58 nm for 2.3 respectively. Solar cells were fabricated with SLAR and DLAR coatings of SiNx:H films and compared the cell efficacy. SiNx:H> films deposited at a substrate temperature of $450^{\circ}C$ and that at 300 W power showed best effective minority carrier lifetime around $50.8\;{\mu}s$. Average reflectance values of SLAR coatings with refractive indices 1.9, 2.05 and 2.3 were 10.1%, 9.66% and 9.33% respectively. In contrast, optimized DLAR coating showed a reflectance value as low as 8.98% in the wavelength range 300nm - 1100nm.

• 전기전자학회논문지
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• 제23권3호
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• pp.1077-1081
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• 2019

태양전지의 표면으로 입사되는 빛은 태양전지의 내부로 모두 흡수되지 못하고 그 일부가 기판 표면에서 반사되어 손실이 발생한다. 때문에 기판 표면의 반사손실을 줄이거나 태양전지 내부의 생성 전하를 증기시키기 위한 연구가 많이 진행 중이다. 본 논문에서는 유리 기판의 표면을 습식 에칭하여 표면을 거칠게 형성하는 표면 처리를 진행하였으며, 거칠어진 표면의 구조적 특성을 분석하였다. 그리고 빛이 입사되는 유리 기판의 각도를 변화하면서 그에 따른 분광특성 또한 분석하였다. 입사되는 빛이 에칭된 표면으로 조사될 때 다중반사에 의해서 유리 기판 내부에 빛을 재흡수할 확률이 증가함을 확인하였다. 또 유리 기판의 각도를 변화하면서 빛을 입사할 때 빛의 투과 및 반사 성능은 변화하지 않음을 확인하였다.

• 한국지구과학회지
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• 제25권7호
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• pp.604-614
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• 2004

경기도 이천에서 2002년 7월부터 12까지 총 6개월 동안 측정된 지자기 3성분 자료를 이용하여 일별 각 성분의 스펙트럼, 지자기 전달함수의 크기, 위상, 오차 등을 계산하였다. 지자기 스펙트럼은 관측기간 동안 태양활동에 의한 무작위적 강약이 반복되는 형태를 보여주었고, 유의미한 시간적 변동은 존대하지 않았다. 지자기 전달함수의 크기, 위상, 오차의 경우, 주기 100초 이하와 주기 1000초 이상에서 부분적으로 무작위적인 경향을 확인할 수 있었으나, 시간에 따른 증감추세 없이 대체로 안정적인 값을 보였다. 이와 더불어, 전기장의 P$_{1}\;^{0}$ 소스(zonal harmonics) 가정을 통하여 시간에 따른 근사적인 겉보기 전기비저항의 변동을 조사하였는데, 근사된 전기비저항의 변화는 지각의 자체적인 물성 변화보다는 수평 자기장 성분의 시간적 강약에 지배적임을 확인할 수 있었다.

• 해양환경안전학회지
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• 제24권2호
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• pp.188-195
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• 2018

본 연구에서는 완도 해역에서 단기적인 수온의 변화에 영향을 주는 요인을 파악하기 위하여 시계열 분석을 실시하였다. Power spectrum 결과에서 기온은 약 24 hr에서 peak를 보였으나 수온과 조위는 약 12 hr 및 24 hr에서 peak가 나타났다. 수온과 조위의 상관성을 파악하기 위해 coherence 분석을 실시한 결과, 두 변수는 반일주기에서 0.92로 높은 상관성을 보였다. 또한 수온의 시 공간적인 분포를 파악하기 위하여 수치실험을 실시하였다. 대조기에는 최강 낙조와 최강 창조 시의 평균 수온차가 $0.3^{\circ}C$인 반면, 소조기에는 평균 수온차가 $0.13^{\circ}C$로 작았다. 대조기의 수온차가 큰 이유는 비교적 수온이 낮은 외해수가 강한 조류에 의해 창조 시 유입되고 낙조 시 빠져나가기 때문인 것으로 판단된다. 전반적으로 수온은 외해보다 연안에서 높게 나타났다. 외해보다 연안은 수심이 얕기 때문에 일사량에 의해 수온이 빠르게 증가하기 때문인 것으로 사료된다.

• 천문학회보
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• 제40권1호
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• pp.86.3-86.3
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• 2015

There could be significant numbers of isolated stellar mass black holes in our Galaxy. The detection of these black holes will provide important clues on the origin of supermassive black holes. Interstellar gas will be accreted to these isolated black holes in nearly spherical flow. The gas and the interstellar magnetic field will be compressed and emit bremsstrahlung and magnetic bremsstrahlung. We calculate the density, temperature, magnetic field of the accretion flow onto a 10 solar mass black hole as well as its radiative emission; special attention is given to cyclotron radiation and synchrotron radiation, which covers from microwave to X-ray. We consider the possibility to detect these radiation from isolated Galactic black holes with current instruments and surveys.

• 한국응용과학기술학회지
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• 제8권1호
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• pp.45-49
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• 1991

The synthesis of urocanic acid which was started D-fructose, and its alkyl esters, urocanic ethyl ester and urocanic isobutyl ester, were prepared by esterificated. Urocanic ethyl ester and urocanic isobutyl ester were insoluble in water and soluble most organic solvents (ethanol, benzene, toluene, pyridine, THF, DMF) which adds to their practical applicability, and absorb ultraviolet light of greater wavelength than the free acid and there by are more effective for shielding sensitive materials, including the humanbody, from the chemically most effective portion of the solar ultraviolet spectrum.