• Journal of Magnetics
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• 제14권1호
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• pp.11-14
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• 2009

We investigated the I-V curves and differential tunneling conductance of two, CoFeB/MgO/CoFeB-based, magnetic tunnel junctions (MTJs): one with a low tunneling magnetoresistance (TMR; 22%) and the other with a high TMR (352%). This huge TMR difference was achieved by different MgO sputter conditions rather than by different annealing or deposition temperature. In addition to the TMR difference, the junction resistances were much higher in the low-TMR MTJ than in the high-TMR MTJ. The low-TMR MTJ showed a clear parabolic behavior in the dI/dV-V curve. This high resistance and parabolic behavior were well explained by the Simmons' simple barrier model. However, the tunneling properties of the high-TMR MTJ could not be explained by this model. The characteristic tunneling properties of the high-TMR MTJ were a relatively low junction resistance, a linear relation in the I-V curve, and conduction dips in the differential tunneling conductance. We explained these features by applying the coherent tunneling model.

• 대한수학회보
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• 제54권5호
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• pp.1597-1617
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• 2017

The paper is devoted to the description of family of scalene triangles for which the triangle formed by the intersection points of bisectors with opposite sides is isosceles. We call them Sharygin triangles. It turns out that they are parametrized by an open subset of an elliptic curve. Also we prove that there are infinitely many non-similar integer Sharygin triangles.

• 지구물리와물리탐사
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• 제17권1호
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• pp.11-20
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• 2014

원주시 저고도 지역에서의 천부 횡파속도($v_s$) 및 부지특성을 파악하기 위해 2013년 2월부터 2013년 9월 사이의 20일간 4.5 Hz 수직 지오폰 12 ~ 24개를 이용하여 원주시계 내의 78 지점에서 레일리파를 기록하였다. 레일리파 분산곡선은 확장된 공간자기상관함수법으로 구하였고, $v_s$를 구하기 위하여 감소최소자승법으로 역산하였다. 이들 1-D 모델로부터 구한 풍화암질 기반암의 깊이($D_b$), 기반암의 횡파속도($v_s^b$), 토양층의 평균 횡파속도($\bar{v}_s^s$), 30 m까지 평균 횡파속도($v_s30$)는 95% 신뢰구간에서 각각 $16.3{\pm}0.7m$, $576{\pm}8m/s$, $290{\pm}7m/s$, $418{\pm}13m/s$로 산출되었다. $v_s30$의 적절한 지시자를 결정하기 위해서 $v_s30$과 지표면 경사도(r = 0.46) 및 고도(r = 0.43)와의 상관계수를 계산하였고, 개별적으로 평가한 $v_s30$과의 상관성을 종합하여 지표면 경사도, 고도, 암상의 가중치를 각각 0.45, 0.45, 0.1으로 하는 선형 경험식을 제시하였다. 그러나 이 경험식과 역산으로 구한 $v_s30$의 상관성이 미약하여(r = 0.50), 적용시에는 상대적으로 큰 오차범위를 고려해야 할 것이다.

• Journal of Astronomy and Space Sciences
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• 제24권2호
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• pp.99-110
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• 2007

W UMa형 접촉쌍성 CC Com을 소백산 천문대에서 61cm 망원경과 2K CCD 카메라로 2002년 3월 3일부터 4월 3일까지 3일간 측광관측하여 총 824개의 관측점(${\Delta}B$: 206점, ${\Delta}V$: 206점, ${\Delta}R$: 206점, ${\Delta}I$: 206점)을 얻었다. 우리의 관측점으로부터 9개의 새로운 극심시각(주극심: 6개, 부극심: 3개)을 산출하였다. 2004년 Wilson-Devinney(WD) 쌍성 모형 계산 프로그램으로 우리가 얻은 새로운 BVRI 광도곡선과 발표된 이중시선속도 곡선들을 결합하여 분석함으로서 CC Com의 제 물리요소를 새롭게 산출하였다. 광도곡선에 나타난 작은 비대칭을 반성에 고온 반점 2개를 도입하여 설명하였다.

• Journal of Astronomy and Space Sciences
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• 제28권2호
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• pp.109-116
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• 2011

The first presented BV light curves of BH UMa confirmed Krajci's (2005) result that BH UMa is an RR Lyr star that belongs to the RRc subgroup. The light curves showed a slight asymmetry of D = 0.453 with an amplitude of about $0.^m58$ in B, $0.^m47$ in V, and $0.^m11$ in B-V and with a small hump between $0.^p82$ and $0.^p86$. We determined nine new times of minimum light and eight times of maximum light. We also analyzed all of the available unanalyzed minimum timings and found for the first time that the period of BH UMa has varied dramatically in at least three independent sinusoidal ways superposed on a secularly downward parabola over 66 years. The secular period decreasing rate was obtained as $6.^d684{\times}10^{-8}y^{-1}$, corresponding to -0.58 s/century. The semi-amplitude and period for each of the three sinusoidal variations were ($0.^d058$, $14.^y44$), ($0.^d044$, $9.^y98$), and ($0.^d005$, $0.^y97$), respectively. It is uncertain whether the periodicity for the shortest period of $0.^y97$ is real or spurious. The secular period decrease, well consistent with those of the other RRc stars, could be considered as a natural result of the evolution of the BH UMa system. The two possible sinusoidal terms were interpreted as both two light-time effects due to two additional bodies orbiting BH UMa and combinations of random fluctuations in the pulsation period of BH UMa. Two interpretations were shortly discussed with related parameters.

• KIEE International Transaction on Electrical Machinery and Energy Conversion Systems
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• 제4B권2호
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• pp.86-91
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• 2004

PV power generation, which directly converts solar radiation into electricity, contains numerous significant advantages. It is inexhaustible and pollution-free, silent, contains no rotating parts, and has size-independent electricity conversion efficiency. The positive environmental effect of photovoltaics is that it replaces the more polluting methods of electricity generation or that it provides electricity where none was available before. This paper highlights a novel simple method to abstract the entire parameters of the solar cell. In development, design and operation of PV power generation systems, a technique for constructing V-I curves under different levels of solar irradiance and cell temperature conditions using basic characteristic values of the PV module is required. Everyone who has performed manual acquisition and analysis of solar cell I versus V data would agree that the job is tedious and time-consuming. A better alternative is to use an automated curve tracer to print out the I versus V curves and compute the four major parameters; $V_{oc}$, $I_{sc}$, FF, and . Generally, the V-I curve tracer indicates only the commonly used solar cell parameters. However, with the conventional V-I curve tracer it is almost impossible to abstract the more detailed parameters of the solar cell; A, $R_{s}$ and $R_{sh}$ , which satisfies the user, who aims at the analysis of the development of the PV power generation system, that being advanced simulation. In this paper, the proposed method provides us with satisfactory results to enable us to abstract the detailed parameters of the solar cell; A, $R_s$ and $R_{sh}$.>.

• 한국물환경학회지
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• 제28권6호
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• pp.917-922
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• 2012

In order to improve applicability of a microbial fuel cell the laboratory-scaled study has been performed by adopting an air-cathode MFC system with high concentrated anaerobic slugies in this study. The concentrations of microbes are grouped into three types, Type A (TS 1.7%), Type B (TS 1.1%) and Type C (TS 0.51%). The open circuit voltage $(V_{oc})$ characteristics showed that the medium microbes concentration of 1.10% (Type B) kept a constant voltage of 1.0 V for 150 hours, which showed the longest time among three types (Type A and Type C). The discharge charge curves for a closed circuit with $500 \Omega$ also showed that Type B generated a stable discharge voltage of 0.8 V for a longer time as in the open circuit voltage case. This could be explained by the relatively large amount of the attached microbes. Under the $V_{oc}$condition the COD removal efficiency of Type B was found to be low for a long time, but those of Type A and C were found to be high for a short period of time. Therefore, the suspended microbes could decrease the coulombic efficiency. It was concluded that the high $V_{oc}$ was caused by low COD and the $V_{oc}$ became low after the COD removal. The COD reduction resulted in an unstable and low working voltage. From the polarization characteristics Type A was found to show the highest power density of $193\;mW/m^2$ with a fill factor of 0.127 due to the relatively high remaining COD even after the MFC reaction.

• Journal of Astronomy and Space Sciences
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• 제3권1호
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• pp.41-51
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• 1986

식쌍성 TX UMa의 2색 (V와 B)의 광천측광에 의한 광도곡선(Oh and Chen 1984)을Wilson and Devinney(1971) 모델에 의한 differential corrections 방법으로 분석하였다. 그결과 TX UMa의 온도가 낮고 질량이 작은 반성은 Roche lobe를 채우고 있는 준접촉 식쌍성으로 해석된다. 한펀, 이번에 얻은 TX UMa의 측광학적 궤도요소와 Hiltner( 1945)의 분광궤도요소로부터 이 별의 절대량을 구하였다. 이에 따르면, 분광형이 B8V인 주성은 core hydrogen burning의 zero age main sequence stage에 있으며 반성은 shell hydorgen burning stage 이후 contraction stage의 진화 상태에 놓여 있는 것으로 추정된다.

• 천문학회지
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• 제39권3호
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• pp.73-80
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• 2006

We analyze the extinction law towards several B1V stars-members of our Galaxy, searching for possible discrepancies from the galactic average extinction curve. Our photometric data allow to build extinction curves in a very broad range: from extreme UV till infrared. Two-colour diagrams, based on the collected photometric data from the ANS UV satellite, published UBV measurements and on the infrared 2MASS data of the selected stars, are constructed. Slopes of the fitted straight lines are used to build the average extinction curve and to search for discrepant objects. The selected stars have also been observed spectroscopically from the Terskol and ESO Observatories; these spectra allow to check their Sp/L's. The spectra of only about 30% of the initially selected objects resemble closely that of HD144470, considered as the standard of B1 V type. Other spectra either show some emission features or belong clearly to another spectral types. They are not used to build the extinction curve. Two-colour diagrams, constructed for the selected B1 V stars, showing no emission stellar features, prove that the interstellar extinction law is homogeneous in the Galaxy. Both the shape of the curve and the total-to-selective extinction ratio do not differ from the galactic average and the canonical value(3.1) respectively. The circumstellar emissions usually cause some discrepancies from the average interstellar extinction law; the discrepancies observed in the extraterrestrial ultraviolet, usually follow some misclassifications.

• Journal of Astronomy and Space Sciences
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• 제6권2호
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• pp.119-125
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• 1989

UBV observations of the primary eclipse of Algol-type long period eclipsing binary AY Persei have been successfully made using the 61-cm reflector at the Ilsan Station of Yonsei University Observatory in September and October, 1989. These light curves furnish ones to deduce following results; (1) the total duration of the eclipse lasted for about 0.066(0.78 days) with no clear evidence of the existence of the totality, (2) the depths of mid-eclipse of $0^m.91$ and $1^m.07$ for V and B, respectively, (3) two times of minimum light, JD2447820.203 and JD 2447820.200 for V and B, respectively, and (4) no period variation with the improved light elements, Min I =JD2427152.237+$11^d.776620e$, $pm$10 $pm$4 are made.