• Proceedings of the Korean Society of Broadcast Engineers Conference
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• 2004.11a
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• pp.259-262
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• 2004

본 논문은 열악한 채널 환경에서 ATSC 방식의 DTV 수신기의 성능 개선을 위해 빔 선택형 DTV 수신기 구조와 최적의 빔 선택을 위한 알고리즘을 제시하고자 한다. 빔 선택형 DTV 수신기의 채널 개선으로 인한 수신기의 성능 개선 효과와 이에 따른 최적 빔 선택을 위한 조건들을 살펴된다. 그리고 필드 테스트를 통해 측정된 ATSC DTV 수신 채널 모델링을 이용하여 등차기만을 사용하는 기존의 DTV수긴기와 빔 선택형 DTV수신기의 성능을 모의 실험을 통해 확인하였다.

• Journal of The Korean Astronomical Society
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• v.34 no.4
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• pp.321-323
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• 2001

Compressible, magnetohydrodynamic (MHD) turbulence in two dimension is studied through high-resolution, numerical simulations with the isothermal equation of state. First, hydrodynamic turbulence with Mach number $(M)_{rms}\;\~$1 is generated by enforcing a random force. Next, initial, uniform magnetic field of various strengths with Alfvenic Mach number Ma $\gg$ 1 is added. Then, the simulations are followed until MHD turbulence is fully developed. Such turbulence is expected to exist in a variety of astrophysical environments including clusters of galaxies. Although no dissipation is included explicitly in our simulations, truncation errors produce dissipation which induces numerical resistivity. It mimics a hyper-resistivity in our second-order accurate code. After saturation, the resulting flows are categorized as SF (strong field), WF (weak field), and VWF (very weak field) classes respectively, depending on the average magnetic field strength described with Alfvenic Mach number, $(Ma)_{rms}{\ge}1$, $(Ma)_{rms}{\~}1$, and $(Ma)_{rms}{\gg}1$. The characteristics of each class are discussed.

• Journal of The Korean Astronomical Society
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• v.34 no.4
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• pp.341-343
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• 2001

Here were continue the MHD study started by Santillan et al (1999) for the interaction of high-velocity clouds (HVCs) with the magnetized thick gaseous disk of our Galaxy. We use the MHD code ZEUS-3D and perform 3D-numerical simulations of this interaction, and study the formation of head-tail structures in HVCs. Our results show that clouds located above 2 kpc from mindplane present velocity and column density gradients with a cometary structure that is similar to those observed in 21 cm emission

• Journal of The Korean Astronomical Society
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• v.37 no.4
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• pp.237-241
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• 2004

We perform numerical experiments on supernova-driven turbulent flows in order to see whether or not supernovae playa major role in driving turbulence in the interstellar medium. In a $(200pc)^3$ computational box, we set up, as initial conditions, uniformly magnetized gas distributions with different pairs of hydrogen number densities and magnetic field strengths, which cover the observed values in the Galactic midplane. We then explode supernovae at randomly chosen positions at a Galactic explosion rate and follow up the evolution of the supernova-driven turbulent flows by integrating numerically the ideal MHD equations with cooling and heating terms. From the numerical experiments we find that the density-weighted velocity dispersions of the flows are in the range of 5-10 km $s^{-l}$, which are consistent with the observed velocity dispersions of cold and warm neutral media. Additionally, we find that strong compressible flows driven by supernova explosions quickly change into solenoidal flows.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.1
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• pp.57.2-57.2
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• 2014

Protostellar jets and outflows are signatures of star formation and promising mechanisms for driving supersonic turbulence in molecular clouds. We quantify outflow-driven turbulence through three-dimensional numerical simulations using an isothermal version of the total variation diminishing code. We drive turbulence in real space using a simplified spherical outflow model, analyze the data through density probability distribution functions (PDFs), and investigate density and velocity power spectra. The real-space turbulence-driving method produces a negatively skewed density PDF possessing an enhanced tail on the low-density side. It deviates from the log-normal distributions typically obtained from Fourier-space turbulence driving at low densities, but can provide a good fit at high densities, particularly in terms of mass-weighted rather than volume-weighted density PDF. We find shallow density power-spectra of -1.2. It is attributed to spherical shocks of outflows themselves or shocks formed by the interaction of outflows. The total velocity power-spectrum is found to be -2.0, representative of the shock dominated Burger's turbulence model. Our density weighted velocity power spectrum is measured as -1.6, slightly less that the Kolmogorov scaling values found in previous works.

• The Bulletin of The Korean Astronomical Society
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• v.41 no.1
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• pp.51.1-51.1
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• 2016

Turbulent motions produce density and magnetic field fluctuations. Correlation between density and magnetic field fluctuations are important for interpretation of observations, such as the rotation measure (RM) and dispersion measure (DM). We study the several factors that can affect the correlation between two. In particular, we numerically investigate how the correlation time of driving affects the correlation between density and magnetic field. We perform compressible MHD turbulence simulations at different sonic Mach number and consider two different driving schemes - continuously changing driving and delta-correlated driving. The continuously changing driving results in strong anti-correlation between density and magnetic field when sonic and Alfvenic Mach numbers are similar unity. The delta-correlated driving produces virtually no correlation between two fields.

• Journal of the Korean Magnetic Resonance Society
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• v.22 no.4
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• pp.144-148
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• 2018

Catalytic enzyme Pyrazinamidase (PncA) from Mycobacterium tuberculosis can hydrolyze substrate pyrazinamide (PZA) to pyrazoic acid (POA) as active form of compound. Using NMR spectroscopy, pH-dependent catalytic properties were monitored including metal binding mode during converting PZA to POA. There seems to be a conformational change through zinc binding in active site from the perturbation of peak intensities in series of 2D HSQC spectra the conformation changes through zinc binding.

• The Bulletin of The Korean Astronomical Society
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• v.44 no.1
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• pp.43.3-43.3
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• 2019

Magnetic fields play an important role in supporting molecular clouds against gravitational collapse. The measured magnetic field strengths in molecular clods enable us to see the effect of magnetic fields in star-forming regions. People have used the Chandrasekhar and Fermi (CF) method to estimate magnetic field strength from observational quantities of molecular cloud density, turbulent velocity and polarization angle dispersion. However, previous studies obtained just one magnetic field strength over the quite large region of a molecular cloud by using the CF method. We here suggest a way to estimate magnetic field strength distribution in Orion A region. We used 450 and 850-micron polarization data of James Clerk Maxwell Telescope (JCMT). Magnetic field strengths were estimated in two wavelengths with 4 pixel resolutions of 16, 20, 24 and 28". Through statistical analysis, we proved the difference of magnetic field strengths between two wavelengths were caused by the difference of their beam sizes. Additionally, we calculated the radii of curvature of polarization segments to select a best pixel resolution for estimating the magnetic field distribution. The pixel resolution should be larger than a radius of curvature. We selected that 20 or 24" pixel resolutions are good choices towards Orion A region.

• KNOM Review
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• v.24 no.2
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• pp.1-12
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• 2021

Recently, research on CBDC (Central Bank Digital Currency) has been actively conducted for various reasons by countries around the world. In addition, with the dazzling development of blockchain technology, blockchain technology is being adopted in CBDC. In this paper, we propose a blockchain-based CBDC system that can be effectively used in the traditional banking system. We also analyze the requirements of CBDC and suggest ways to commercialize CBDC. We present a system design and implementation method, especially in terms of compatibility, interoperability, and privacy.

• Proceedings of the Korean Society of Computer Information Conference
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• 2022.01a
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• pp.203-207
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• 2022

모바일 결제시스템의 다양한 특성에 힘입어 많은 사용자는 언제 어디서나 시간과 장소의 제약에서 벗어나 다양한 제품을 손쉽게 구매할 수 있게 되었다. 이러한 측면에서 본 연구는 모바일 결제시스템 사용자들의 특성(인구통계적 특성, 모바일 결제시스템 이용특성)에 따라 모바일 결제시스템이 갖추어야 하는 특성(보안성, 호환성, 효율성, 경제성, 신뢰성)에 대한 인식도가 어떻게 달라지는가를 실증적으로 규명하고자 하였다. 한국과 중국의 모바일 결제시스템 사용자들을 대상으로 설문지를 활용한 실증분석을 실시한 결과, 사용자들의 성별과 국적에 따라 모바일 결제시스템의 일부 특성에 대한 인식도에 있어서 차이가 존재하고 있음을 확인하였다.