• 한국항해항만학회지
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• 제26권2호
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• pp.245-259
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• 2002

1978년 7월 1일부로 발효된 국제안전관리규약에 해당되는 선박과 회사는 안전관리시스템을 구축하고, 실행하고, 유지하여야 한다. 그러나 아직까지는 이 제도가 정착되지 못한 실정이다. 이 논문은 현행 안전관리시스템상의 문제점을 도출하고 그 개선방안을 제시하고자 한다.

• 한국항해항만학회:학술대회논문집
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• 한국항해항만학회 2013년도 춘계학술대회
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• pp.441-442
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• 2013

ISM Code 1.2.2.2항 개정안 발효됨에 따라 선박에서 실질적으로 위험성평가 (Risk Assessment) 시행을 요구하고 있다. 하지만 해운업계 및 선원들은 관련 지식 및 경험 부족으로 시행에 여러움을 겪고 있다. 이 연구에서는 선상에서 효과적인 이행을 위해 표준 위험성평가 지침을 개발하였다.

• 천문학회보
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• 제44권2호
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• pp.47.2-47.2
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• 2019

Observations indicate that turbulence in molecular clouds of the interstellar medium (ISM) is highly supersonic (M >> 1) and strongly magnetized (β ≈ 0.1), while in the intracluster medium (ICM) it is subsonic (M <~1) and weakly magnetized (β ≈ 100). Here, M is the turbulent Mach number and β is the ratio of the gas to magnetic pressures. Although magnetohydrodynamic (MHD) turbulence in such environments has been previously studied through numerical simulations, some of its properties as well as its consequences are not yet fully described. In this talk, we report a study of MHD turbulence in molecular clouds and the ICM using a newly developed code based the high-order accurate, WENO (Weighted Essentially Non-Oscillatory) scheme. The simulation results using the WENO code are generally in agreement with those presented in the previous studies with, for instance, a TVD code (Porter et al. 2015 &, Park & Ryu 2019), but reveal more detailed structures on small scales. We here present and compare the properties of simulated turbulences with WENO and TVD codes, such as the spatial distribution of density, the density probability distribution functions, and the power spectra of kinetic and magnetic energies. We also describe the populations of MHD shocks and the energy dissipation at the shocks. Finally, we discuss the implications of this study on star formation processes in the ISM and shock dissipation in the ICM.

• 대한전자공학회:학술대회논문집
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• 대한전자공학회 2003년도 통신소사이어티 추계학술대회논문집
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• pp.285-288
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• 2003

Code Select CDMA(CS/CDMA)(1)는 입력 데이터 열에 의하여 여러 채널의 직교코드를 선택하여 전송하는 기술로, 멀티코드 CDMA 의 구조를 가지면서도 전송신호의 크기가 일정하여 저가의 비선형 증폭기를 사용하여 구현 할 수 있다. 특히 입력 비트열을 부호화하여 직교코드들의 합을 일정하게 만드는 constant amplitude coded (CA-) CS/CDMA (2) 전송 기술은 2.4GHz ISM 대역의 WPAN을 위한 전송방식의 하나로 고려되고 있다. 이주파수 대역은 WLAN, 블루투스 등을 비롯한 여러 시스템이 존재하는 대역이므로 다른 종류의 시스템과의 상호 간섭의 문제를 분석할 필요가 있다. 본 논문에서는 2.4GHz ISM 대역을 같이 사용하게 될 IEEE 802.11b WLAN 과 CA-CS/CDMA 기반의 WPAN 상호 영향을 물리계층 측면에서 분석한다. IEEE 802.11b 모델로 11MHz 대역폭을 갖는 CCK (Complementary Code Keying) 변조방식을 대상으로 하며, CA-CS/CDMA 와의 중심주파수 차이에 따른 비트오율 성능을 신호대 간섭전력의 비를 변화시켜가면서 컴퓨터 모의실험을 통하여 분석하였다.

• 천문학회지
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• 제37권4호
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• pp.137-141
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• 2004

We have estimated the fractal dimension of the molecular clouds in the Antigalactic Center based on the $^{12}CO$ (J = 1- 0) and $^{13}CO$ (J = 1- 0) database obtained using the 14m telescope at Taeduk Radio Astronomy Observatory. Using a developed code within IRAF, we were able to identify slice-clouds, and determined the dispersions of two spatial coordinates as well as perimeters and areas. The fractal dimension of the target region was estimated to be D = 1.34 for low resolution $^{12}CO$ (J = 1 - 0) database, and D = 1.4 for higher resolution $^{12}CO$ (J = 1 - 0) and $^{13}CO$ (J = 1 - 0) database, where $P {\propto} A^{D/2}$. The sampling rate (spatial resolution) of observed data must be an important parameter when estimating fractal dimension. Our database with higher resolution of 1 arcminute, which is corresponding to 0.2 pc at a distance of 1.1 kpc, gives us the same estimate of fractal dimension to that of local dark clouds. Fractal dimension is apparently invariant when varying the threshold temperatures applied to cloud identification. According to the dispersion pattern of longitudes and latitudes of identified slice-clouds, there is no preference of elongation direction.

• 천문학회지
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• 제49권6호
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• pp.255-259
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• 2016

We estimate the fractal dimension of the ${\rho}$ Ophiuchus Molecular Cloud Complex, associated with star forming regions. We selected a cube (${\upsilon}$, l, b) database, obtained with J = 1-0 transition lines of $^{12}CO$ and $^{13}CO$ at a resolution of 22" using a multibeam receiver system on the 14-m telescope of the Five College Radio Astronomy Observatory. Using a code developed within IRAF, we identified slice-clouds with two threshold temperatures to estimate the fractal dimension. With threshold temperatures of 2.25 K ($3{\sigma}$) and 3.75 K ($5{\sigma}$), the fractal dimension of the target cloud is estimated to be D = 1.52-1.54, where $P{\propto}A^{D/2}$, which is larger than previous results. We suggest that the sampling rate (spatial resolution) of observed data must be an important parameter when estimating the fractal dimension, and that narrower or wider dispersion around an arbitrary fit line and the intercepts at NP = 100 should be checked whether they relate to firms noise level or characteristic structure of the target cloud. This issue could be investigated by analysing several high resolution databases with different quality (low or moderate sensitivity).

• 천문학회지
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• 제41권6호
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• pp.157-161
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• 2008

We have estimated the fractal dimension of the molecular clouds associated with the Hii region Sh 156 in the Outer Galaxy. We selected the $^{12}CO$ cube data from the FCRAO CO Survey of the Outer Galaxy. Using a developed code within IRAF, we identified slice-clouds (2-dimensional clouds in velocity-channel maps) with two threshold temperatures to estimate the fractal dimension. With the threshold temperatures of 1.8 K, and 3 K, we identified 317 slice-clouds and 217 slice-clouds, respectively. There seems to be a turn-over location in fractional dimension slope around NP (area; number of pixel) = 40. The fractal dimensions was estimated to be D = $1.5\;{\sim}\;1.53$ for $NP\;{\geq}\;40$, where $P\;{\propto}\;A^{D/2}$ (P is perimeter and A is area), which is slightly larger than other results. The sampling rate (spatial resolution) of observed data must be an important parameter when estimating fractal dimension. Fractal dimension is apparently invariant when varying the threshold temperatures applied to slice-clouds identification.

• 천문학회보
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• 제42권2호
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• pp.43.1-43.1
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• 2017

A three-dimensional (3D) $Ly{\alpha}$ radiative transfer code is developed to study the Wouthuysen-Field effect, which couples the 21 cm spin temperature of neutral hydrogen and the $Ly{\alpha}$ radiation field, and the escape fraction of $Ly{\alpha}$ from galaxies. The Monte Carlo code is capable of treating arbitrary 3D distributions of $Ly{\alpha}$ source, neutral hydrogen and dust densities, gas temperature, and velocity field. It is demonstrated that the resonance-line profile at the center approaches to the Boltzmann distribution with the gas temperature. A plane-parallel ISM model, which is appropriate for the neutral ISM of our Galaxy, is used to calculate the $Ly{\alpha}$ radiation field strength as a function of height above the galactic plane. We also use a two-phase, clumpy medium model which is composed of the cold and warm neutral media (WNM). It is found that the $Ly{\alpha}$ radiation field is strong enough to thermalize the 21 cm spin temperature in the WNM to the gas kinetic temperature. The escape fraction of $Ly{\alpha}$ is found to be a few percent, which is consistent with the $Ly{\alpha}$ observations of our Galaxy and external galaxies.

• 한국산업정보학회논문지
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• 제19권1호
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• pp.13-18
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• 2014

무선 센서 네트워크에서 센서 노드는 주변 환경을 감시하고 데이터를 수집하는 용도로 사용되고 있다. 여러 센서 노드들로 구성된 센서 네트워크는 유비쿼터스 컴퓨팅 분야에 핵심 기술로 주목 받고 있다. 센서 노드는 수집된 정보를 처리하기 위한 MCU와 작은 용량의 메모리를 가지고 있다. 배터리로 동작하는 센서 노드는 한번 배치되면 추가적인 에너지 공급이 불가능하기 때문에 전원 관리 능력이 반드시 필요하다. 또한 ISM 밴드 대역의 주파수를 사용하고 다수의 센서 노드들이 배치된 장소에서 동작하여야 하기 때문에 같은 센서 노드와 같은 대역을 사용하는 이종 기기간의 전파 간섭이 발생하는 열악한 통신환경에서 가지고 있다. 본 논문에서는 무선 센서 네트워크의 오류 제어 기법으로 사용되는 ARQ 기법의 문제점인 오류가 발생 했을 시 재전송으로 인한 추가적인 에너지 소비를 줄이기 위해 오류정정기법인 컨벌루션 부호의 적용을 제안하였다. 제안된 컨벌루션 부호를 센서 네트워크 OS를 통하여 센서 노드에 적용하여 전송전력 -19.2dbm과 -25dbm 에서 거리를 10m, 15m, 20m로 두고 BER을 측정하였다. 측정된 BER을 통해 패킷손실률과 평균 재전송 횟수를 계산하여 컨벌루션 부호를 적용하였을 때 그 성능을 분석하였다. 실험결과 -19.2dbm에서는 9~12%의 평균 재전송 횟수 이득을 -25dbm에서는 12%~19%의 이득을 얻을 수 있음을 확인하였다.

• 천문학회보
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• 제35권2호
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• pp.71.1-71.1
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• 2010

The far-ultraviolet (FUV) C IV and H2 emission spectra of Orion-Eridanus Superbubble (OES) is hereby presented. The OES seems to consist of multiple phase through the detection of highly-ionized gas and pervasive neutral hydrogen. The former is traced by hot gas while the latter is traced by cold medium. A spectral image made with H2 fluorescent emission shows that the spatial distribution of hydrogen molecule is well correlated with the dust map. The model spectra was taken from a photodissociation region (PDR) radiation code which finds a best suitable parameter such as hydrogen density and intensity of the radiation field. C IV emission is caused by intermediate temperature ISM about 10^5 K. Therefore we could get more clear evidence to reveal the morphology of OES. In this process, the hydrogen density and gas temperature were also estimated. The data were obtained with the Far-Ultraviolet Imaging Spectrograph (FIMS) and the whole data handling were followed by previous FIMS analysis.