• 대한의용생체공학회:학술대회논문집
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• 대한의용생체공학회 1998년도 추계학술대회
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• pp.185-186
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• 1998

The discrete Wigner-distribution(DWD) was implemented for the time-frequency analysis of heart rate variability signals. The smoothed cross-DWD was used to estimate time-varying power spectrum. Spurious cross-terms were suppressed using a smoothing data window and a Gauss frequency window. The DWD is very easy to implement using the FFT algorithm. Experiment show that the DWD follows well the instantaneous changes of spectral content of heart rate variability signals, which characterize the dynamics of autonomic nervous system response.

• 한국전기전자재료학회:학술대회논문집
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• 한국전기전자재료학회 2007년도 추계학술대회 논문집
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• pp.377-378
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• 2007

In this paper, we were confirmed the optical characteristics of LED module by changing ambient temperature and driving current. When we supplied same driving current, the brightness quality drops due to an increased ambient temperature. The difference of brightness properties came out more large according to an increased driving current. Moreover, peak wavelength become shifted by long wavelength and declined output power by increasing driving current.

• 천문학회보
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• 제40권2호
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• pp.42.1-42.1
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• 2015

We model the Spectral Energy Distribution (SED) of Class 0 protostar L1527 IRS using a radiative transfer code RADMC-3D. In addition to the photometry data from literatures, we include the Herschel/PACS data which well covers the far-infrared SED peak of L1527 IRS, providing precise constraints to the density structure and other physical properties of its circumstellar envelope. Previously, Tobin et al. (2013) presented a dust continuum modeling results using a rotating and infalling envelope (Terebey and Shu, & Cassen 1984 ; TSC envelope), which originally describes a power-law density profile (${\rho}{\propto}r-{\alpha}$) with the power-law index (${\alpha}$) of 1.5. However, we find that Herschel/PACS data are better fitted with a shallower power-law density profile. This smaller power-law might be attributed to a inner envelope. Thus, we fit the SED of L1527 IRS with a Bonnor-Ebert sphere, which is a combination of the inner flat-topped and the outer power-law (${\alpha}=2$) density profiles. This Bonnor-Ebert sphere is often used to explain the density profile of prestellar cores, which is considered the earliest stages of star formation. The well-fitted SED with a Bonnor-Ebert sphere suggests that L1527 IRS might have collapsed from a Bonnor-Ebert sphere rather than a singular isothermal sphere.

• 대한기계학회논문집
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• 제18권5호
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• pp.1253-1263
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• 1994

The experimental study is carried out to identify the combustion generated noise mechanism in free turbulent jet diffusion flames. Axial mean fluctuating velocities in cold and reacting flow fields were measured using hot-wire anemometer and LDv.The overall sound pressure level and their spectral distribution in far field with and without combustion were also measured in an anechoic chamber. The axial mean velocity is 10-25% faster and turbulent intensities are about 10 to 15% smaller near active reacting zone than those in nonreacting flow fields. And sound pressure level is about 10-20% higher in reacting flow fields. It is also shown that the spectra of the combustion noise has lower frequency characteristics over a broadband spectrum. These results indicate that the combustion noise characteristics in jet diffusion flames are dominated by energy containing large scale eddies and the combusting flow field itself. Scaling laws correlating the gas velocity and heat of combustion show that the acoustic power of the combustion noise is linearly proportional to the 3.8th power of the mean axial velocity rather than 8th power in nonreacting flow fields, and the SPL increases linearly with logarithmic 1/2th power of the heat of combustion.

• 전자공학회논문지S
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• 제34S권2호
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• pp.79-93
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• 1997

This paper presents a linear shift-invariant system euqivalent to morphological dilation for a memoryless uniform source in the sense of the power spectral density function, and comares it with dialtion. This equivalent LSI system is found through spectral decomposition and, for dilation and with windwo size L, it is shown to be a finite impulse response filter composed of L-1 delays, L multipliers and three adders. Th ecoefficients of the equivalent systems are tabulated. The comparisons of dilation and its equivalent LSI system show that probability density functions of the output sequences of the two systems are quite different. In particular, the probability density functon from dilation of an independent and identically distributed uniform source over the unit interval (0, 1) shows heavy probability in around 1, while that from the equivalent LSI system shows probability concentration around themean vlaue and symmetricity about it. This difference is due to the fact that dilation is a non-linear process while the equivalent system is linear and shift-ivariant. In the case that dikation is fabored over LSI filters in subjective perforance tests, one of the factors can be traced to this difference in the probability distribution.

• Journal of Astronomy and Space Sciences
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• 제33권2호
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• pp.109-117
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• 2016

We explain the results of Yu et al. (2015b) of the novel sharpness angle measurement to a large number of spectra obtained from the Fermi gamma-ray burst monitor. The sharpness angle is compared to the values obtained from various representative emission models: blackbody, single-electron synchrotron, synchrotron emission from a Maxwellian or power-law electron distribution. It is found that more than 91% of the high temporally and spectrally resolved spectra are inconsistent with any kind of optically thin synchrotron emission model alone. It is also found that the limiting case, a single temperature Maxwellian synchrotron function, can only contribute up to 58⁺²³₋₁₈% of the peak flux. These results show that even the sharpest but non-realistic case, the single-electron synchrotron function, cannot explain a large fraction of the observed spectra. Since any combination of physically possible synchrotron spectra added together will always further broaden the spectrum, emission mechanisms other than optically thin synchrotron radiation are likely required in a full explanation of the spectral peaks or breaks of the GRB prompt emission phase.

• 천문학회보
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• 제37권1호
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• pp.76.2-76.2
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• 2012

The understanding spectral characterization of possible earth-like extra solar planets has generated wide interested in astronomy and space science. The technical central issue in observation of exoplanet is deconvolution of the temporally and disk-averaged spectra of the exoplanets. The earth model based on atmospheric radiative transfer method has been studied in recent years for solutions of characterization of earthlike exoplanet. In this study, we report on the current progress of the new method of 3D earth model as a habitable exoplanet. The computational model has 3 components 1) the sun model, 2) an integrated earth BRDF (Bi-directional Reflectance Distribution Function) model (Atmosphere, Land and Ocean) and 3) instrument model combined in ray tracing computation. The ray characteristics such as radiative power and direction are altered as they experience reflection, refraction, transmission, absorption and scattering from encountering with each all of optical surfaces. The Land BRDF characteristics are defined by the semi-empirical "parametric-kernel-method" from POLDER missions from CNES. The ocean BRDF is defined for sea-ice cap structure and for the sea water optical model, considering sun-glint scattering. The input cloud-free atmosphere model consists of 1 layers with vertical profiles of absorption and aerosol scattering combined Rayleigh scattering and its input characteristics using the NEWS product in NASA data and spectral SMARTS from NREL and 6SV from Vermote E. The trial simulation runs result in phase dependent disk-averaged spectra and light-curves of a virtual exoplanet using 3D earth model.

• Transactions on Electrical and Electronic Materials
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• 제3권4호
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• pp.21-26
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• 2002

Color correction methods of chromaticity coordinates using Color Matching Function (CMF) were studied to develop a device-independent portable-type urine analyzer. The reflection spectra were measured for the degrees of 10 test items of the urine reagent strip (urine strip) to develop a portable-type urine analyzer. A computer simulation was performed to quantitatively distinguish the color reactions of the urine system, by using the spectral power distribution of Light Emitting Diode(LED), the reflection of a urine strip, and spectral sensitivity of a photodiode. To develop a device-independent system, chromaticity coordinates were modified to reduce the color deviations in the urine strip, by using the temperature compensation of LED and the color transformation by CMF. The experimental values obtained by developed urine system exhibited the accuracy above 95% for all color samples.

• 한국통신학회논문지
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• 제40권1호
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• pp.240-245
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• 2015

본 연구는 디밍 요구 사항 하에서 가시광 통신 시스템의 다양한 이진 변조 방식들에 대한 플리커 효과의 영향에 대해 분석하였다. 기존의 플리커에 관한 분석 연구는 신호의 통계만을 고려하여 플리커의 동적 현상을 효과적으로 기술하지 못하였으나 본 연구에서는 전력 스펙트럼을 적절히 이용하여 가시광 신호에 대한 저주파 플리커의 영향을 비교 분석하였다. 그 결과, 플리커 측면에서는 변조 방식들 중 아날로그 디밍이 우수하며 또한 신호의 파형 및 분포에 대한 처리를 통해 플리커를 완화할 수 있음을 확인하였다.

• 지구물리와물리탐사
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• 제10권4호
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• pp.241-251
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• 2007

본격적인 지진관측 이래 최대 규모의 내륙 지진으로 기록된 오대산지진의 관측 스펙트럼을 이용하여, 점지진원 스펙트럼 모델의 지진원 크기 및 오차의 공간적인 특성을 평가하였다. 먼저 지진원 스펙트럼을 추정하기 위해, 최근까지 국내에 축적된 지진자료를 기반으로 비교적 상세하게 추정된 추계학적 지진동모델(Boore, 2003)의 지진파 전달, 부지특성(연관희, 2007)을 이용하여 관측 자료를 보정하였다. 추정된 오대산지진의 지진원 스펙트럼을 $1-f_c$(1개의 코너주파수) Brune의 ${\omega}^2$ 지진원모델에 적합한 결과, 기존에 제시된 지진규모-응력강하량 대표모델(연관희 등, 2006)에 의해 잘 예측되었으며, 오대산지진의 지진원 스펙트럼은 최근까지 한반도 인근에서 발생한 중규모 이상의 지진원 스펙트럼으로부터 추정된 $2-f_c$(2개의 코너주파수)의 경험적인 지진원모델에 보다 잘 부합되었다. 또한 일반적으로 무작위 잡음으로 취급되는 점지진원 지진파 스펙트럼 모델링 오차에 대해 방위각에 따른 방향성과 지역별 전달특성을 평가한 결과, 오차가 완전한 무작위 특성이 아님을 확인할 수 있었다. 이러한 모델링 오차의 방향성은 이론적으로 추정된 방사패턴과도 매우 유사한 관측된 방사패턴을 나타내었으며, 지역별로는 지질학적인 경계 혹은 지진파전달의 불연속적 특성과 밀접한 관계가 있는 것으로 판단되는 주파수별로 상이한 공간적인 분포 특성을 보여주었다.