본 연구는 적충복합보에 있어서의 층간분리현상을 추적하는 기법을 소개하고 있다. 이 기볍에서는 충간분 리된 보와 층간분리되지 않은 보와의 응답차이를 최대화하도록 조화운동의 가력올 보위별로 최적화한다.2개 층의 알루미늄 보에 대하여 수치해석을 수행하였으며， 계측 및 보의 형태에 따른 노이즈를 고려하였다. 층간 분리를 모텔링하기 위하여 스웹함수를 사용하였으며 층별복합판 이론에 기본한 유한요소법을 이용하여 해석 하였다.

We have analyzed vector magnetograms and Hβ filtergrams of two sunspot groups, one in a growing phase and the other in a decaying phase. In this study, the temporal evolution of their magnetic morphology has been investigated in association with solar activity. The morphological variations of the growing and decaying phase of these sunspots revealed in detail the coalescence of small spots into a large spot and the fragmentation of a large spot into many small spots, respectively. Numerous small flares were detected in the spot group during the decaying phase. This seems to be intimately associated with the shearing motions of many spots with different polarities created by fragmentation of a large sunspot. The magnetic flux and the average shear angle are found to be substantially reduced during the decaying phase, especially in the course of the flarings. This implies that the decaying phase of the sunspot is, to some degree, involved with magnetic field cancellation. The growing spot group has not shown any large activities, but numerous small spots have grown into a typical bipolar sunspot.

한 cycle 의 이력곡선 loop을 완전히 표현하기 위해서는 pinch force, drift offset, effective stiffness, 따ùoading， reloading, tangential stiffness 둥의 변수가 펼요하게 된다. 각 이력 loop에 대해 이들 변수들은 에너지 소산정도에 따라 변위와 축력의 함수로 표현될 수 있다. 본 논문에서는 먼저 16개의 전단벽 실험에서 얻어진 이력곡선 데이타를 분석하여 앞에 기술된 모든변수를 표준화된 변위(ð./ð.y) 의 함수로 표현했으며 이 를 바탕으로 이력콕선의 포락선으로 표현되는 힘-변위관계를 예측할 수 있는 6개의 step올 제시하였다. 제시 된 기볍으로 구해진 비탄성 힘 변위관계는 실험곡선과 비교되었으며 내진설계에 있어서 가장 중요한 요소중 하나인 구조물의 비탄성 힘-변위관계를 예측하는 편리한 기법으로 이용될 수 있음을 보였다.

이 연구의 목적은 단조하중과 반복하중올 받는 철근콘크리트 면부재 해석에 대한 이방향성 회전 직교촉 모 텔의 성능올 검토하기 위함이다. 여기서 다루는 구조부재는 철근에 의하여 적절히 보강된 보， 기퉁， 보-기둥 접합부， 그리고 전단벽둥으로 부재의 파괴가 인장균열후 압축파괴에 의하여 일어나는 부재이다. 보통 단조하 중에 대하여 사용도는 이방향성 회전 직교축 모텔을 반복하중에 대하여 확장하며， 철근파 부착의 기존 재료모 델과 함께 유한요소해석에 사용한다. 단조하중에 대하여 이방향성 회전 직교축 모델올 사용한 해석 결과는 취 성파괴를 나타내는 철근콘크리트보의 실험결과와 비교된다. 또한 반복하중올 받는 전단벽의 극한하중， 비선 형 변형， 핀칭 현상동에 대하여 실험결과와비교된다.

구조물의 최적설계에 대한 일반적인 개념이 제시되며 Gradient Projection법과 설계민감도 해석을 사용한 최 적 화 알고리즘이 논의된다. 6충 평면 철 골 구조물 의 최소무게 설 계의 예 를 통해 이 알고리즘의 적용올 예시 한다. 시스댐 전 체의 비용분석뿐만 아니라 임계 비용 및 설계민 감도 해석파 같은 이 알고리즘의 장점에 관하 여 설명한다3

An attempt has been made to analyze time series of Hα, Hβ, and Hɤ line profiles taken from a 3B/X6.1 flare which occurred on Oct. 27, 1991 in an active region, NOAA 6891. A total of 22 sets of Hα, Hβ, and Hɤ taken with a low and non-uniform time resolution of 10-40 seconds were scanned by PDS with absolute intensity calibration to derive the physical characteristics of the material in the flare chromosphere. Our . results are as follows: (1) The lower Balmer lines observed during the flare activity are broadened by Stark effect. (2) At the peak of the flare activity, the electron temperature of the Balmer line emitting region reaches up to 35000K and its geometrical thickness increases to a scale of ~104km, suggesting that high energy particles penetrate deep into the photospheric level.

앞의 논문 Part 1 에서 유도한 변분원리를 이용하여 복합재료적충판의 진동해석을 할 수 있는 유한요소해 석 모델을 개발하였다. 이 모델에서는 어느 한 충의 면내 변위와 나머지층 단연의 회전각， 그리고 판 전체의 연직방향처짐을 절점변수로 취하게 되어 n개층으로된 적충판의 경우 2(n+ 1) +1 의 절점 자유도를 갖는다. 따 라서， 판의 주변에서는 한층의 면내변위와 각충단연의 회전각을， 판의 면내에서는 연직방향 처짐을 경계조건 값으로 정의할 수 있다. 이 모델에 의해 개발한 프로그램을 이용하여 각층의 재료특성이 크게 다환 혼종형 복 합재료적충판 (hybrid laminate) 의 고유진동문제를 해석하였다. 탄성이론해 빛 다른 유한요소해석결과와 본 해석결과와의 비교를 통해 제시모델이 기존의 다른 유한요소모델보다 정확함올 예시하였다.

적층판의 동적거동에 대한 유한요소해석모텔개발을 목적으로 전단변형을 적합하게 고려한 적층판이론에 대한 변분원리를 유도하였다. 유도방볍은 Sandhu 동에 의해 개발된 다변수 경계치문제의 변분원리이론을 따 았으 며， 지배방정식의 미분연산자 매트릭스를 self-adjoint로 만들기 위하여 convolution을 이중선형사상으로 사용하였다 유도된 적충판의 범함수에는 경계조건， 초기조건쁜만 아니라 유한요소해석모텔에서 생길 수 있 는 요소간 불연속조건도 포함시킬 수 있다. 상태변수의 적합함수공간을 확장하거나 특정조건을 적용하브로서 다양한 형태의 범함수를 유도할 수 있으며， 이를 통해 다양한 유한요소해석모델의 개발이 가능함을 논하였다.

We propose to use the entropy of power spectra defined in the frequency domain for the deconvolution of extended images. Spatial correlations requisite for extended sources may be insured by increasing the role of power entropy because the power is just a representation of spatial correlations in the frequency domain. We have derived a semi-analytical solution which is found to severely reduce computing time compared with other iteration schemes. Even though the solution is very similar to the well-known Wiener filter, the regularizingng term in the new expression is so insensitive to the noise characteristics as to assure a stable solution. Applications have been made to the IRAS 60μm and 100 μm images of the dark cloud B34 and the optical CCD image of a solar active region containing a circular sunspot and a small pore.

We have analyzed a set of high resolution photographic line profiles of a Zeeman sensitive Fe I λ 6302.5 line taken with the Universal Birefringent Filter over a single round sunspot (SPO 5007) at the Sacramento Peak Solar Observatory. The observed spectra recorded on films are traced by PDS and the traced densities are converted to relative intensity by means of IRAF. The Stokes I and V profiles are then constructed by adding together and subtracting from each other the left and right handed circular polarizations, respectively. The reduced I and V profiles are analyzed by means of the coarse analysis(Auer et al.(1977), Skumanich and Lites(1987)) with the use of inversion technique. It is found that the umbral field strength is about 3000 gauss and the field distribution follows closely the emperical model proposed by Wittmann(1974).

Magnetostatic models of starspots of late type main sequence stars ( G 5 V \~ K 5 V ) have been constructed to investigate their physical characteristics by using the similarity law suggested by Schluter and Temesvary(1958) and later employed by Deinzer(1965) and Yun(1968). The starspots are assumed to be single, circular and in horizontal magnetostatic equilibrium. In the present study we considered only those model spots whose area covers less than 12 % of the entire stellar surface as suggested by observations. The computed surface field strength of our model spots ranges from 10 3 \;to\;several\;10^3$ gauss and their magnetic flux is found to be 10 \~ 100 times that of sunspots. The field strength is sensitive to spectral type, which increases with later spectral type. In contrast to the field strength, the area of starspots depends strongly on the total magnetic flux. Finally, it is noted that the computed field strength of model spots belonging to G 0 V \~ G 5 V falls below the equipartition field strength at their parent stellar surface unless the coverage is less than 2 % . This suggests that the observed spot on G 0 V \~ G 5 V stars is likely to be a group of small starspots.

We have conducted surface photometry of a spiral galaxy NGC4419, by making use of photographic plates in U, B, V and R-bands taken by 105cm Schmidt Camera at Kiso Observatory. Two dimensional surface brightness distributions as well as luminosity profiles along the major axis are examined in detail to decipher the morphological properties of the galaxy. Analysis of the color distributions of NGC4419 shows that B-V and U-B colors remain constant throughout the galaxy with a weak trend of blue bulge in B-V color. The blue bulge might indicate an active star formation in the nucleus of NGC4419. For a quantitative analysis of the luminosity distribution of NGC4419, the observed luminosity profiles are decomposed into bulge and disk components, assuming the bulge component to follow de Vaucouleurs γ 1 / 4 − l a w while the disk component is assumed to be exponential. The fitting generally fails at the central part and at the shoulder near r = 15' where bulge and disk components overlap. The failure at the central part cannot be attributed wholly by the seeing disk since the core-radius of the central plateau is much larger than the width of point spread function. The failure at shoulder could be due to the luminosities from the spiral arms.

We have conducted BVI photographic surface photometry of four spiral galaxies NGC1087, NGC2715, NGC2844 and NGC3593, by making use of the Kiso Schmidt plates. Detailed examination of the morphological properties of the galaxies using isophotal maps and luminosity profiles showed that all the program galaxies have some peculiarities in their luminosity distributions. NGC1087 and NGC2715 have extremely small nuclei with inner rings which contain several bright HII regions. NGC2844 has a very large bulge whose luminosity dominates over the disk luminosity in all the radii. The I-band luminosity profile of NGC3593 shows shallower gradient than B- and V-band profiles. We were able to successfully decompose the luminosity profile into a bulge following de Vaucouleurs γ 1 / 4 − l a w and an exponential disk only for NGC 3953. Other galaxies have more complicated luminosit profiles.

Technology is unevenly distributed across countries, thus constituting an entry barrier. Under several simplifying assumptions, technology licensing strategies among incumbent and entrant firms in the intermational context are analyzed. First, in a model with two monopolistic firms, the conditions for licensing to occur are elaborated as a function of the costs of the two firms. Licensing is likely to occur only when the entrant has a more competitive cost position than the incumbent to compensate for the royalty payment. However, if the incumbent has much lower marginal cost than the entrant, the incumbent has an incentive not to license the technology. Second, a new set of issues arises when multiple potential licensors are considered. The maximum and minimum values of the royalty payment decrease as the number of incumbents with the technology increases. Moreover, each incumbent has an incentive to sell the technology before other incumbents do, which leads to a Prisoner`s Dilemma situation. Third, in the case of multiple licensees, a potential entrant`s willingness to pay for a license depends upon the strategies of other firms. The optimal pricing strategy of the licensor is identified.