• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2003년도 한국우주과학회보 제12권2호
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• pp.39-39
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• 2003

The plasmaspheric region shows relatively strong longitudinal asymmetry in the sense that the location of the plasmapause and the density distribution significantly vary with respect to local time, and this asymmetry effect has been neglected in previous magnetospheric ULF wave studies. In this study, we numerically examine the MHD wave properties of field line resonances (FLRs) and Pi2 pulsations when the inner magnetosphere is assumed to be asymmetric. We use the dipole magnetic field model, but our density model is based on. observational data from the IMAGE satellite. We assume an impulsive input in the magnetotail, which can be associated with a substorm onset. Our results suggest that local FLRs appear in both the radial and azimuthal oscillations owing to the asymmetry. Plasmaspheric Pi2 signals appear in the compressional component, but they are more strongly affected by ambient plasmaspheric structure than the FLRs. We compare our results with the observational data of Pi2 events.

• 천문학회보
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• 제37권2호
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• pp.110.1-110.1
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• 2012

We studied the source regions of 12 solar energetic particle (SEP) events seen between 2010 August and 2012 January at STEREO-A, B and ACE, when the two STEREO spacecraft were separated by about $180^{\circ}$. All events were associated with strong flares (C1 - X6) and fast coronal mass ejections (CMEs) accompanied by type II radio bursts. We have determined the arrival times of the SEP events at the three spacecraft. EUV waves observed in $195{\AA}$ and $193{\AA}$ channels of STEREO and SDO/AIA are tracked across the Sun and the arrival time of the EUV wave at the photospheric source of open field lines extending to the spacecraft connection points at 2.5 Rsun estimated. We found 7 events with flux enhancements in all spacecraft and 4 in two spacecraft. Most events came from a single source. The results show that magnetic field connections between source regions and the spacecraft play an important role in abrupt flux enhancements. In the most cases, EUV waves at the Sun are associated with a wide longitudinal spread of the SEPs.

• 한국자기학회지
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• 제19권2호
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• pp.52-56
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• 2009

[CoFe/Cu/CoFe]/IrMn 다층박막에 대하여 자유층 CoFe 두께에 따른 상호교환결합력, 교환결합세기, 보자력, 자기저항비, 자장감 응도 등의 자기저항 특성을 관찰하였다. IrMn 층을 통해 유도된 강자성체/비자성체/강자성체 구조인 CoFe(t)/Cu($25\;{\AA}$)/CoFe($60\;{\AA}$)/IrMn($80\;{\AA}$) 다층박막은 자유층 CoFe 두께 $30\;{\AA}$일 때 작은 보자력과 높은 자장감응도를 유지하는 연자성 특성을 보였다. 반면에 자유층 CoFe 두께 $90\;{\AA}$일 때 큰 보자력과 낮은 자장감응도를 보였다. 양호한 연자성 특성을 갖은 $2{\times}8{\mu}m^2$ 크기의 CoFe($30\;{\AA}$)/Cu($25\;{\AA}$)/CoFe($60\;{\AA}$)]/IrMn($80\;{\AA}$) 스핀밸브 소자를 제작하였다. 길이방향의 센싱전류와 폭방향의 고정층의 용이축 방향을 택하여 2 단자법으로 측정한 소자의 연자성 자기저항 특성인 자기저항비와 자장감응도는 각각 3.0%와 0.3%/Oe 이었다.

• 한국방재학회 논문집
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• 제9권6호
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• pp.11-15
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• 2009

최근 국내에서는 PSC(Prestressed Concrete) 박스 거더 교량의 교폭을 늘리고 자중을 줄이기 위한 목적으로 박스의 수를 줄이는 대신 콘크리트 충진 FRP(Concrete Filled FRP, CFFRP) 스트럿을 상판 캔틸레버 부분에 설치하는 공법이 시공되고 있다. 이러한 CFFRP 스트럿은 사례가 많지 않은 교량 구조물로서 설계 및 시공에서의 불확실성을 제거하기 위해 교량 시스템에서의 스트럿 거동을 실험적으로 분석할 필요가 있다. 따라서 본 연구에서는 대상교량에 대해 현장시험을 실시하여 CFFRP 스트럿의 국부 거동을 분석하고자 한다. 특히 전자기파 간섭에 대해 면역이 우수한 광센서인 FBG(fiber Bragg grating) 센서를 기반으로 시험을 실시하여 잡음이 없는 우수한 응답을 성공적으로 획득하였다. 현장시험에서는 재하트럭의 속도와 횡방향 위치를 매개변수로 시험을 실시하였다. 그 결과 CFFRP 스트럿은 하중재하 위치와 속도에 관계없이 압축상태에 존재하고 있으며, 통과 차량의 횡방향 위치가 CFFRP 스트럿의 거동에 민감한 요소임을 확인하였다.

• 한국구조물진단유지관리공학회 논문집
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• 제27권6호
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• pp.193-200
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• 2023

본 논문에서는 전자기장 노출을 통한 강섬유의 방향 정렬 방법이 휨파괴거동에 미치는 영향을 비교, 분석하였다. 강섬유의 방향을 휨공시체의 종방향으로 정렬할 수 있는 규모의 솔레노이드를 설계, 제작하였다. 설계강도 30MPa의 강섬유보강콘크리트 휨공시체를 제작하였으며, 이를 전자기장에 노출한 공시체와 노출하지 않은 공시체로 구분하여 휨파괴 실험을 수행하였다. 실험변수는 강섬유의 혼입률과 형상비로 하였다. 실험결과, 전자기장에 노출된 시험체의 휨강도, 최대하중에서의 개구변위가 미소하게 증가하였으며, 특히 파괴에너지의 증가가 명확하게 확인되었다. 잔존강도의 증가가 파괴에너지 증가에 가장 큰 영향을 준 것으로 확인되었다.

• 천문학회지
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• 제28권1호
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• pp.89-95
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• 1995

We examined a total of 166 images of $3.5{\mu}m\;H_3^+$ emission in the auroral regions of Jupiter observed with the Protocam on IRTF in 1991 and 1992, and found that 30 images contain a clearly isolated small emission patch in the vicinity of the northern auroral regions. Two different time sequences of the images show the small patches at the dusk limb in the range of System III longitudes from $270^{\circ}\;through\;0^{\circ}\;to\;90^{circ}$. The small patches in one sequence of the images, which were taken at 10 phase between $240^{\circ}\;and\;260^{\circ}$, may be related to the 10 flux tube, similarly suggested by Connerney et al. (1993). However, the small patches in the other sequence are separated from Io as much as $80^{\circ}$ in longitude. The positions of the small patches in both sequences are deviated equatorward from the 10 footprint oval by $5^{\circ}-8^{\circ}$ latitude in the longitudinal range of $270^{\circ}-360^{\circ}$. A significant modification is required in current Jovian magnetic field models near the Jupiter's surface if the small patches are produced at the foot of the 10 flux tube.

• Smart Structures and Systems
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• 제22권1호
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• pp.105-120
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• 2018

In this paper, the nonlinear free and forced vibration responses of sandwich nano-beams with three various functionally graded (FG) patterns of reinforced carbon nanotubes (CNTs) face-sheets are investigated. The sandwich nano-beam is resting on nonlinear Visco-elastic foundation and is subjected to thermal and electrical loads. The nonlinear governing equations of motion are derived for an Euler-Bernoulli beam based on Hamilton principle and von Karman nonlinear relation. To analyze nonlinear vibration, Galerkin's decomposition technique is employed to convert the governing partial differential equation (PDE) to a nonlinear ordinary differential equation (ODE). Furthermore, the Multiple Times Scale (MTS) method is employed to find approximate solution for the nonlinear time, frequency and forced responses of the sandwich nano-beam. Comparison between results of this paper and previous published paper shows that our numerical results are in good agreement with literature. In addition, the nonlinear frequency, force response and nonlinear damping time response is carefully studied. The influences of important parameters such as nonlocal parameter, volume fraction of the CNTs, different patterns of CNTs, length scale parameter, Visco-Pasternak foundation parameter, applied voltage, longitudinal magnetic field and temperature change are investigated on the various responses. One can conclude that frequency of FG-AV pattern is greater than other used patterns.

• 한국재료학회지
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• 제12권3호
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• pp.195-199
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• 2002

Planar Hall effect of ferromagnetic GaMnAs thin films was investigated for the first time. The films were grown in an optimized growth condition via molecular beam epitaxy at low temperatures. For the optimization of the growth conditions, we used reflection high-energy electron diffraction, electrical conductivity, double crystal x-ray diffraction, and superconducting quantum interference device measurements techniques. We observed that the difference between the longitudinal resistance and the transverse resistance matches the planar Hall resistance. The ratio of the planar Hall resistance at saturation magnetic field to that at zero reached above 500%.

• Journal of Magnetics
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• 제14권1호
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• pp.36-41
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• 2009

Magneto-optical Kerr effect (MOKE) magnetometry was used to investigate magnetization reversal dynamics in 30-nm NiFe/15-nm FeMn, 15-nm FeMn/30-nm CoFe bilayers, and 30-nm NiFe/(2,10)-nm FeMn/30-nm CoFe trilayers. The in-plane magnetization components of each ferromagnetic layer, both parallel and perpendicular to the applied field, were separately determined by measuring the longitudinal and transverse MOKE hysteresis loops from both the front and back sides of the film for an oblique incident s-polarized beam. The magnetization of the FeMn/CoFe bilayer was reversed abruptly and symmetrically through nucleation and domain wall propagation, while that of the NiFe/FeMn bilayer was reversed asymmetrically with a dominant rotation. In the NiFe/FeMn/CoFe trilayers, the magnetic reversal of the two ferromagnetic layers proceeded via nucleation and domain wall propagation for 2-nm FeMn, but via asymmetric rotation for 10-nm FeMn. The exchange-biased ferromagnetic layers showed the magnetization reversal along the same path in the film plane for the decreasing and increasing field branches from transverse MOKE hysteresis loops, which can be qualitatively explained by the theoretical model of the exchange-biased ferromagnetic/antiferromagnetic systems.

• 천문학회지
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• 제24권2호
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• pp.129-149
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• 1991

An attempt has been made to examine the characteristics of acoustic and MHD waves generated in stellar convection zones($4000\;K\;{\leq}\;T_{eff}\;{\leq}\;7000\;K$, $3\;{\leq}\;\log\;g\;{\leq}\;4.5$). With the use of wave generation theories formulated for acoustic waves by Stein (1967), for MHD body waves by Musielak and Rosner (1987, 1988) and for MHD tube waves by Musielak et al.(l989a, 1989b), the energy fluxes are calculated and their dependence on effective temperature, surface gravity and megnetic field strength are analyzed by optimization techniques. In computing magneto-convection models, the effect of magnetic fields on the efficiency of convection has been taking into account by extrapolating it from Yun's sunspot models(1968; 1970). Our study shows that acoustic wave fluxes are dominant in F and G stars, while the MHD waves dominant in K and M stars, and that the MHD wave fluxes vary as $T_{eff}^4{\sim}T_{eff}^7$ in contrast to the acoustic fluxes, as $T_{eff}^{10}$. The gravity dependence, on the other hand, is found to be relatively weak; the acoustic wave fluxes ${\varpropto}\;g^{-0.5}$, the longitudinal tube wave fluxes ${\varpropto}\;g^{0.3}$ and the transverse tube wave fluxes ${\varpropto}\;g^{0.3}$. In the case of the MHD body waves their gravity dependence is found to be nearly negligible. Finally we assesed the computed energy fluxes by comparing them with the observed fluxes $F_{ob}$ of CIV(${\lambda}1549$) lines and soft X-rays for selected main sequence stars. When we scaled the corrected wave fluxes down to $F_{ob}$, it is found that these slopes are almost in line with each other.