• 한국추진공학회지
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• 제6권1호
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• pp.63-70
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• 2002

본 연구에서는 초음속 및 음속 마이크로 제트 유동의 특성을 파악하기 위해서 2차원 축대칭 압축성 Navier-Stokes 방정식을 이용한 수치해석을 수행하였다. 수치해석에서는 여러 형태의 난류모델을 적용하여 실험결과와 비교하였으며, 부족팽창과 과팽창 상태를 얻기 위하여 노즐 출구의 압력비 $P_b/P_e$를 0.2~l.25로 변화시켰다. 또, 레이놀즈 수 Re를 약 600~40000까지의 범위에서 변화시켜, $P_b/P_e$와 Re가 마이크로 제트 유동장에 미치는 영향을 조사하였다. 본 연구로부터 층류 제트의 특성은 난류 제트와는 달리 레이놀즈 수의 의존성이 크다는 것을 알았다.

• 천문학논총
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• 제30권2호
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• pp.481-483
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• 2015

Multi-dimensionality in the inner working of core-collapse supernovae has long been considered one of the most important ingredients to understand the explosion mechanism. We perform a series of numerical experiments to explore how rotation impacts the 3-dimensional hydrodynamics of core-collapse supernova. We employ a light-bulb scheme to trigger explosions and a three-species neutrino leakage scheme to treat deleptonization effects and neutrino losses from the neutron star interior. We find that the rotation can help the onset of neutrino-driven explosions for models in which the initial angular momentum is matched to that obtained from recent stellar evolutionary calculations (${\sim}0.3-3rad\;s^{-1}$ at the center). For models with larger initial angular momenta, a shock surface deforms to be oblate due to larger centrifugal force. This makes a gain region, in which matter gains energy from neutrinos, more concentrated around the equatorial plane. As a result, the preferred direction of the explosion in 3-dimensional rotating models is perpendicular to the spin axis, which is in sharp contrast to the polar explosions around the axis that are often obtained from 2-dimensional simulations.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2010년도 한국우주과학회보 제19권1호
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• pp.25.1-25.1
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• 2010

This talk outlines the current understanding of solar flares, mainly focusing on magnetohydrodynamic (MHD) processes. A flare causes plasma heating, mass ejection, and particle acceleration that generates high-energy particles. The key physical processes related to a flare are: the emergence of magnetic field from the solar interior to the solar atmosphere (flux emergence), formation of current-concentrated areas (current sheets) in the corona, and magnetic reconnection proceeding in current sheets that causes shock heating, mass ejection, and particle acceleration. A flare starts with the dissipation of electric currents in the corona, followed by various dynamic processes which affect lower atmospheres such as the chromosphere and photosphere. In order to understand the physical mechanism for producing a flare, theoretical modeling has been developed, in which numerical simulation is a strong tool reproducing the time-dependent, nonlinear evolution of plasma before and after the onset of a flare. In this talk we review various models of a flare proposed so far, explaining key features of these models. We show observed properties of flares, and then discuss the processes of energy build-up, release, and transport, all of which are responsible for producing a flare. We come to a concluding view that flares are the manifestation of recovering and ejecting processes of a global magnetic flux tube in the solar atmosphere, which was disrupted via interaction with convective plasma while it was rising through the convection zone.

• 한국정보디스플레이학회:학술대회논문집
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• 한국정보디스플레이학회 2005년도 International Meeting on Information Displayvol.I
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• pp.489-492
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• 2005

We report new polymer stabilized ferroelectric liquid crystal (PSFLC) cells with mechanical stability which is achievable by introducing photospacers in the cells. It was found that the mechanical st ability of the PSFLC cell was effected by introduction of photo spacers. We analyzed the dependence of mechanical stability and memory property on the density of photospacers in the PSFLC cell. The stability and memory properties of PSFLC Cells depending on photospacer density are discussed. 1. Introduction Recently, flexible displays have attracted much attention because they have remarkable advantages: thinner, lighter, non-breakable and conformable features. Flexible displays have various potential applications such as e-book and e-paper displays utilizing the distinct features. E-book and E-paper displays demand very low power consumption, so that bistable memory liquid crystal modes are required in case of flexible plastic LCDs for those application. Three kinds of memory LC modes have been developed; bistable nematic, bistable cholesteric and bistable FLC. Among them SSFLC as one of bistable FLC has big advantages such as low driving voltage, wide view angle and fast response time, SSFLC cells are, however, very weak against mechanical shock. Polymer stabilized FLC (PSFLC) has been developed to overcome the poor mechanical stability of SSFLC. PSFLC was known to have network structure that FLCs are oriented with smectic layer ordering in polymer network. The polymer network stabilizes the FLC orientation, which leads to improvement of mechanical stability of PSFLCD. A lot of studies have been done for the application of PSFLC to flexible $LCDs.^{[1{\sim}12]}$ However, it should be noted that PSFLC does not have sufficient mechanical stability for the particular applications such as smart card LCD, where LCD is highly bendable.Bead spacer was mainly used to maintain cell gap of conventional PSFLCDs. But the spacer density of it is not locally uniform in the cell, so that it is generally difficult that the PSFLCDs with bead spacers show sufficient mechanical stability. In order to more improve the mechanical stability of PSFLCDs, we introduced photospacers into PSFLCDs. In this paper, we describe the improvement of mechanical stability by introducing photospacers into PSFLCDs.

• 항공우주시스템공학회지
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• 제14권5호
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• pp.33-41
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• 2020

항공기의 착륙장치는 지상에서 동체로 전달되는 충격에너지를 흡수 및 소산시키는 장치이다. 착륙장치 중 반능동형 MR 댐퍼 착륙장치는 다양한 착륙조건에서 높은 충격흡수효율을 보여주며 제어 불능 시 안정성을 확보할 수 있는 장점이 있다. 오리피스가 아닌 환형 관유로를 이용하는 MR 댐퍼 착륙장치의 경우, 유로 압력강하로 인해 발생하는 감쇠력이 MR 댐퍼 내부 형상 구조에 따라 저압 챔버에서 캐비테이션을 유발할 수 있어 기존의 2 자유도계 모델링 기법보다 다중물리시스템 해석 프로그램인 Amesim이 더 유용하다. Amesim을 이용한 해석결과를 바탕으로 착륙장치 내부 유로 형상 배치를 수정하여 캐비테이션을 방지할 수 있는 유로 구조를 제안하였고 낙하 시험 시뮬레이션 결과를 통해 이를 검증하였다. 본 논문에서는 환형 관로 형태 유로 구조를 갖는 MR 댐퍼형 착륙장치의 캐비테이션 발생시 주요 특성을 파악하였고, 아울러 내부형상 배치 수정을 통해 이를 방지하는 방안을 제시하였다.

• 한국음향학회지
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• 제38권4호
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• pp.459-466
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• 2019

투명한 PMMA (Poly methyl methacrylate) 기판 위에 탄소나노튜브(Carbon Nanotube, CNT)와 PDMS (Poly dimethylsiloxane)를 코팅한 복합체에 레이저 펄스를 조사하면 열탄성효과에 의해 수중에 강한 초음파가 발생한다. 본 논문에서는 그 초음파 발생과 관련한 열음향 이론을 정립하고, 가우시안 파형을 갖는 레이저 펄스를 두께가 $20{\mu}m$인 CNT/PDMS 복합체에 조사했을 때 어떤 파형의 초음파가 발생하는지를 시뮬레이션을 통해 파악하였다. 그 결과로부터 CNT/PDMS 복합체에서는 충격 초음파가 발생하며, 그 파의 형상은 복합체의 각종 물성 값이 ${\pm}20%$ 변하여도 크게 변하지 않는 것을 확인하였다. 그러나 정(+), 부(-)의 피크 값은 열팽창계수가 증가하거나 밀도, 열용량, 음속이 감소하면 증가하며, 열전도도에 대해서는 민감하게 변하지 않음을 알았다. 나아가, 직접 제작한 CNT/PDMS 복합체에서 방사되는 초음파의 측정 결과와 시뮬레이션 결과의 비교로부터 그 물성 값을 추정할 수 있었다.

• Bulletin of the Korean Chemical Society
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• 제33권9호
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• pp.2883-2889
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• 2012

LL-37 is the only antimicrobial peptide (AMP) of the human cathelicidin family. In addition to potent antimicrobial activity, LL-37 is known to have the potential to inhibit lipolysaccharide (LPS)-induced endotoxic effects. To provide the stability to proteolytic digestion and increase prokaryotic selectivity and/or anti-endotoxic activity of two Lys/Trp-substituted 19-meric antimicrobial peptides (a4-W1 and a4-W2) designed from IG-19 (residues 13-31 of LL-37), we synthesized the diastereomeric peptides (a4-W1-D and a4-W2-D) with D-amino acid substitution at positions 3, 7, 10, 13 and 17 of a4-W1 and a4-W2, respectively and the enantiomeric peptides (a4-W1-E and a4-W2-E) composed D-amino acids. The diastereomeric peptides exhibited the best prokaryotic selectivity and effective protease stability, but no or less anti-endotoxic activity. In contrast, the enantiomeric peptides had not only prokaryotic selectivity and anti-endotoxic activity but also protease stability. Our results suggest that the hydrophobicity and ${\alpha}$-helicity of the peptide is important for anti-endotoxic activity. In particular, the enantiomeric peptides showed potent anti-endotoxic and LPS-neutralizing activities comparable to that of LL-37. Taken together, both a4-W1-E and a4-W2-E holds promise as a template for the development of peptide antibiotics for the treatment of endotoxic shock and sepsis.

• Journal of Astronomy and Space Sciences
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• 제29권1호
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• pp.51-55
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• 2012

A few high-mass X-ray binaries-consisting of an OB star plus compact companion-have been observed by Fermi and ground-based Cerenkov telescopes like High Energy Stereoscopic System (HESS) to be sources of very high energy (VHE; up to 30 TeV) ${\gamma}$-rays. This paper focuses on the prominent ${\gamma}$-ray source, LS 5039, which consists of a massive O6.5V star in a 3.9-day-period, mildly elliptical ($e{\approx}0.24$) orbit with its companion, assumed here to be an unmagnetized compact object (e.g., black hole). Using three dimensional smoothed particle hydrodynamics simulations of the Bondi-Hoyle accretion of the O-star wind onto the companion, we find that the orbital phase variation of the accretion follows very closely the simple Bondi-Hoyle-Lyttleton (BHL) rate for the local radius and wind speed. Moreover, a simple model, wherein intrinsic emission of ${\gamma}$-rays is assumed to track this accretion rate, reproduces quite well Fermi observations of the phase variation of ${\gamma}$-rays in the energy range 0.1-10 GeV. However for the VHE (0.1-30 TeV) radiation observed by the HESS Cerenkov telescope, it is important to account also for photon-photon interactions between the ${\gamma}$-rays and the stellar optical/UV radiation, which effectively attenuates much of the strong emission near periastron. When this is included, we find that this simple BHL accretion model also quite naturally fits the HESS light curve, thus making it a strong alternative to the pulsar-wind-shock models commonly invoked to explain such VHE ${\gamma}$-ray emission in massive-star binaries.

• 천문학회지
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• 제47권6호
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• pp.259-277
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• 2014

G192.8-1.1 has been known as one of the faintest supernova remnants (SNRs) in the Galax until the radio continuum of G192.8-1.1 is proved to be thermal by Gao et al. (2011). Yet, the nature of G192.8-1.1 has not been fully investigated. Here, we report the possible discovery of faint non-thermal radio continuum components with a spectral index ${\alpha}{\sim}0.56(S_{\nu}{\propto}{\nu}^{-{\alpha}})$ around G192.8-1.1, while of the radio continuum emission is thermal. Also, our Arecibo $H_I$ data reveal an $H_I$ shell, expanding with an expansion velocity of $20-60km\;s^{-1}$, that has an excellent morphological correlation with the radio continuum emission. The estimated physical parameters of the $H_I$ shell and the possible association of non-thermal radio continuum emission with it suggest G192.8-1.1 to be an~0.3 Myr-old SNR. However, the presence of thermal radio continuum implies the presence of early-type stars in the same region. One possibility is that a massive star is ionizing the interior of an old SNR. If it is the case, the electron distribution assumed by the centrally-peaked surface brightness of thermal emission implies that G192.8-1.1 is a "thermal-composite" SNR, rather than a typical shell-type SNR, where the central hot gas that used to be bright in X-rays has cooled down. Therefore, we propose that G192.8-1.1 is an old evolved thermal-composite SNR showing recurring emission in the radio continuum due to a nearby massive star. The infrared image supports that the $H_I$ shell of G192.8-1.1 is currently encountering a nearby star forming region that possibly contains an early type star(s).

• 한국추진공학회지
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• 제7권4호
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• pp.33-38
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• 2003

플룸간섭 현상은 플룸에 의한 경계층 유동의 박리, 강한 전단층의 발생, 그리고 다수의 충격파들이 박리유동 및 전단층과 상호작용하게 되는 매우 복잡한 유동현상으로, 현재 미사일의 후미부에서 발생하는 플룸간섭 현상의 상세에 관해서는 잘 알려져 있지 않다. 본 연구에서는 초음속 미사일의 동체후미부에서 발생하는 플룸간섭 현상의 특징 및 동체기저부에 설치된 다공확장벽(porous extension)의 플룸간섭 현상에 대한 영향을 수치해석적으로 조사하였다. 그 결과, 다공확장벽이 플룸에 의한 충격파와 경계층 유동의 박리를 완화시켜 미사일 동체의 제어성능이 향상될 수 있음을 알았다.