• The Transactions of the Korean Institute of Power Electronics
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• v.11 no.6
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• pp.502-507
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• 2006

According to large-sized LCD, the CCFL used in backlight is getting longer and a backlight using one lamp makes a needed brightness by arranging lamp in parallel because of the limit of brightness. In this paper, the inverter to nu the large back-light in 42inch LCD TV using 20 CCFLs was designed to produce the same output on each lamp in any input condition. Supplementing the conventional high-low method driving CCFL, by adopting high-high one, the brightness variation among each lamp sides is improved. Additionally, to improve the brightness variation, the method connecting the lamp and the capacitor in series is used. The proposed system was verified by the experiment.

• Journal of The Korean Astronomical Society
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• v.50 no.4
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• pp.105-109
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• 2017

The well-known solar cycle controls almost the entire appearance of the solar photosphere. We therefore presume that the continuous emission of visible light from the solar surface follows the solar cyclic variation. In this study, we examine the solar cyclic variation of photospheric brightness in the visible range using solar images taken by the Solar and Heliospheric Observatory (SOHO)/Michelson Doppler Imager (MDI). The photospheric brightness in the visible range is quantified via the relative intensity acquired from in the raw solar images. In contrast to total solar irradiance, the relative intensity is out of phase with the solar cycle. During the solar minimum of solar cycles 23-24, the relative intensity shows enhanced heliolatitudinal asymmetry due to a positive asymmetry of the sunspot number. This result can be explained by the strength of the solar magnetic field that controls the strength of convection, implying that the emission in the visible range is controlled by the strength of convection. This agrees with the photospheric brightness increasing during a period of long spotless days.

• Journal of Broadcast Engineering
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• v.7 no.4
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• pp.291-299
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• 2002

This paper proposes an efficient motion compensation algorithm for video sequences with brightness variations. In the proposed algorithm, the brightness variation parameters are estimated and local motions are compensated. To detect the frame with large brightness variations. we employ the frame classification based on the cross entropy between histograms of two successive frames, which can reduce the computational redundancy. Simulation results show that the proposed method yields a higher peak signal to noise ratio (PSNR) than the conventional methods, with a low computational load, when the video scene contains large brightness changes.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.2
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• pp.52.1-52.1
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• 2010

The Japanese infrared (IR) space mission AKARI monitored the brightness in the fields very close to the north ecliptic pole (NEP) with nine wavebands in Infrared Camera (IRC), which cover the wavelength range from 2 to $24{\mu}m$. We reduced the NEP monitor observations and examined the smoothness of the sky background brightness. Our analysis shows that the background brightness is smooth over a frame of about $10'\times10'$ within about 0.1% deviation in mid-IR. Because the zodiacal light (ZL) and emission (ZE) dominate the diffuse sky brightness in the near- and mid-IR wavelengths, the background brightness varies with season through a year. We tried sinusoidal fittings to the observed NEP background brightness. The fitting analysis shows that the sine function is successful in describing the seasonal variation of the ZL and ZE within 2% deviations from the observed brightness, especially for the 15, 18, and $24{\mu}m$ bands, within 0.3%. These results will provide limits and caveats for the studies of the cosmic infrared background radiation.

• Proceedings of the KIEE Conference
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• 2001.07d
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• pp.2585-2587
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• 2001

This paper suggests a method of color variation technique to generate stable white light. The light from high brightness RGB LED was mixed according to the RGB LED luminance ratio. A microcontroller-based PWM control circuit and switching circuit is used to achieve full color variation. It is confirmed that the stable white light and full color variation is possible.

• Journal of The Korean Astronomical Society
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• v.22 no.2
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• pp.141-160
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• 1989

In order to derive time dependence of the atmospheric diffuse light, which consists of the airglow continuum emission and diffusely scattered radiations of the intergrated starlight, the diffuse Galactic light, and the zodiacal light, we have analyzed the meridian scan observations of the sky brightness at $5,080\;{\AA}$ and $5,300\;{\AA}$. Amplitude of the time-variation becomes larger for lower elevation, and maximum amplitude is found to be about $50\;S_{10}(V)_{G2V}$ at elevation $10^{\circ}$. The atmospheric diffuse radiation attains maximum brightness at around midnight, and afterward it decreases slowly with time. The time-variations for the two wavelengths are similar to each other. The observed brightness distribution of the diffuse light along the zenith distance is fitted to an empirical relation of two parameters. By making the two parameters time-dependent, we describe the spatial and time variations of the atmospheric diffuse light. This enables us to make time dependent correction for the atmospheric diffuse component in the reduction of zodiacal light brightness.

• Proceedings of the KSRS Conference
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• 2005.10a
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• pp.370-373
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• 2005

We have developed Hybrid algorithm for yellow sand detection. Hybrid algorithm is composed of three methods using infrared bands. The first method used the differential absorption in brightness temperature difference between $11\mu m\;and\;12\mu m$ (BID _1), through which help distinguish the yellow sand from various meteorological clouds. The second method uses the brightness temperature difference between $3.7\mu m\;and\;11\mu m$ (BID_2). The technique would be most sensitive to dust loading during the day when the BID _2 is enhanced by reflection of $3.7\mu m$ solar radiation. The third one is a newly developed algorithm from our research, the so-called surface temperature variation method (STY). We have applied the three methods to MODIS for derivation of the yellow sand dust and in conjunction with the Principle Component Analysis (PCA), a form of eigenvector statistical analysis. PCI shows better results for yellow sand detection in comparison with the results from individual method. The comparison between PCI and MODIS aerosols optical depth (AOD) shows remarkable good correlations during daytime and relatively good correlations over the land.

• Publications of The Korean Astronomical Society
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• v.30 no.2
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• pp.269-270
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• 2015

We carried out near-IR photometric and optical spectroscopic observations of V582 Aur, which is a FU Orionis type object, to investigate any periodic and/or aperiodic variations. We obtained light curves on the scale of a night and a year, in J, H and Ks bands with KASINICS (KASI Near Infrared Camera System) attached to the BOAO (Bohyun-san Optical Astronomy Observatory) 1.8-m reflector in Youngcheon, South Korea and examined photometric variations on the two time scales. So far we have not found any periodic brightness variations on the scale of a night. On the other hand, we have found that there seems to be a periodic brightness variation with a period of approximately 45 days. In addition, high-resolution optical spectroscopic observations of V582 Aur were performed from February 2013 to May 2014 with the high-resolution echelle spectrograph BOES attached to the BOAO 1.8-m reflector. We analyzed several spectral lines to understand the physical state of V582 Aur. The P Cyg profiles are clearly shown in the $H{\alpha}$ line and Na I D line.

• Publications of The Korean Astronomical Society
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• v.5 no.1
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• pp.85-94
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• 1990

Wangjo Silok, the official chronicle of Lee Dynasty, carries 131 records on the Kepler Supernova 1604; all of them are given in the present report. Among them 112 records are detailed descriptions about the observed brightness variation over the period from October 13, 1604 (the 37th year of King Sunjo) to April 23, 1605. On July 14, 1605, an addendum is given as a final assessment of the guest star incidence. Since the apparent brightness, size and position are carefully described as compared to bright planets and stars, these records are ideal for retrieving light curve of the Kepler Supernova over the seven month period. Simple procedures are suggested for the derivation of light curve.

• Journal of the Korea Academia-Industrial cooperation Society
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• v.7 no.6
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• pp.1028-1033
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• 2006

In general the cooling of projection TV is realized with aluminum coupler and coolant. A new type of projection TV with plastic coupler is discussed. Compared with an aluminum coupler, the plastic coupler has the advantage of cost, but is not as good as aluminum one in cooling performance. Therefore it is thought that there may be some problems such as brightness degradation induced by insufficient cooling andit is needed to investigate the relation between phosphor brightness and temperature variation. In this paper, a procedure is developed to predict the brightness degradation of CRT in projection TV with plastic coupler. Thermal analysis for CRT in projection TV is performed using FEM (finite element method).