본 연구에서는 지하암반구조물의 구조해석시 불연속암반체의 물성변이를 고려할 수 있는 확률론적해석기범을 개발하였다. 수치해석적 접근은 몬테칼로모사기법의 단점을 보완한 LHS기법을 사용하였고, 불연속변의 영향은 단층,벽개 등과 같이 불연속성이 뚜렷한 지역에서 적용성이 높은 절리유한요소모델을 사용하였다. 재료특성에 대한 확률변수는 불연속변의 수직강성과 전단상성을 다확률변수로 사용하였으며, 이들은 확률공간에 정규분포를 갖는 경우에 대하여 고려하였다. 본 연구에서 개발된 수치해석프로그램은 검증예제를 통하여 타당성을 확인하였으며, 가상의 불연속면군의 존재하는 지하원형공동에 대한 해석을 통하여 프로그램의 적용성을 확인하였다.

The luminosity function (LF) and present day mass function(PDMF) for main sequence (MS) stars in the Praesepe and Hyades clusters are derived, showing the Wielen Dip which occurs at Mv = 9m in the LF. This dip is about 2 mag fainter than the case for the Pleiades cluster whose Wielen Dip position is consistent with that for the solar neighborhood field stars. The Wielen Dips of these clusters are reproduced by using a bimodal initial mass function (IMF).

The prevention of oxidative degradation in fats and oils is largely controlled by the use of synthetic phenolic antioxidants. Antioxidants, BHA: 2-&3-tert-butyl-4-hydroxyanisol, BHT: 3,5-di-tert-butyl-4-hydroxytoluene, TBHQ: tert-butylhydroquinone, PG: propyl gallate, PTG: pentyl gallate, OG: octyl gallate, were extracted from fatty foods with hexane and from hexane layer to presaturated acetonitrile with hexane. The polar phenolic hydroxyl groups of antioxidants were silylated with MSTFA and injected to Gas Chromatography/Mass Spectrometry. The calibration plots were linear in the investigated range, 0.1-10.0 ug/g. The limit of detection for 6 phenolic antioxidants was 0.1 ug/g. Recoveries and reproducibilities from samples fortified at 1.0 ug/g were in the range of 70-90% and 0.5-13%, respectively. The simultaneous determination of phenolic antioxidants in fatty foods using GC/MS-SIM mode and macro program was described.

본 논문은 집중 질량 구조물의 천이응답에 대한 시간영역 민감도 해석의 기본 개념을 설명한다. 외부 가진에 따른 구조물의 응답에 미치는 설계변수 변화의 영향을 구하기 위해 시간영역 민감도 함수를 구하는 방법을 제시하였다. 시간영역에서 구조물의 설계변수 민감도는 1차 표준 민감도 함수와 백분율 민감도 함수를 통해 확인하였다. 이러한 민감도 함수와 그 계산은 설계변수에 대한 시스템 상태변수의 편미분에 의한 것이다. 또한, 직접 미분법에 의한 해석적 방법의 편미분 결과와 수치적 방법에 의한 결과를 비교하였다.

본 논문은 첨가질량이 있는 양단 단순지지 타단 자유단의 경계조건을 갖는 특별 직교 이방성 적층복합판에 대한 적용례로 제시한다. 구조물 설계시 설계자들은 구조물의 정확한 고유진동수를 계산할 필요성을 느끼나 정확한 해답을 얻기란 매우 어렵다. Pretlove는 유효질량 개념을 사용하여 첨가질량을 갖는 보의 해석 방법을 발표하였다. 그러나 이 방법은 단순보의 경우에만 유용할 뿐이다. 그러므로 본 논문에선 해석법이 간단하고, 정확하며, 임의의 경계조건과 단면을 가진 판의 해석에 매우 효과적인 김덕현의 방법으로 첨가질량이 있는 적층복합판의 고유진동수를 계산하였다.

The case for a massive black hole in the center of the Galaxy is reassessed using improved modeling techniques and observational data. A dark mass of ~2 ×10 6 M⊙ is present within 0.2 pc of the Galactic center. However, the available data can be modeled, without appealing to a massive black hole, using an extended distribution of dark stellar remnants (neutron stars and stellar mass black holes) provided that the stellar initial mass function in the central parsec is deficient in stars less massive than ~1 M⊙. Such a situation may be a natural consequence of repeated gas build-up followed by starbursts in the central region. A clear distinction between this and the massive central black hole model cannot be made using red giant tracers outside 0.2 pc due to uncertainties in the radial velocity dispersion distribution. The cluster of massive early-type emission-line stars in the central parcsec more effectively probe the mass distribution close to Sgr A *, but their small number and partial rotational support complicate mass determinations. Proper motion determinations for stars within 0.5' of Sgr A * may be the most effective means of unambiguously determining the mass distribution in the immediate vicinity of the Galactic center.

This study was designed to investigate food consumption patterns and nutrient intakes of college students, divided into subgroups of normal weight men (no.=140), normal weight women (no.=101), and underweight women (no.=155) by body mass index. Frequency of food eaten, nutrient intakes from each meal, percentages of RDAs, and nutrient densities were analyzed using 24-hour recall records. It was very interesting in these results as follows. Normal weight men ate on the whole more frequently than other groups. Underweight women had higher intakes of nutrient than did normal weight women. However normal weight women consumed food of greater nutrient density than did other college students. Consequently, it is desirable to suggest nutrient density of food than learn RDAs for adequate diet in nutritional education programs.

31 white dwarfs in 10 open clusters are examined, and their maximum mass and the upper mass limit of their progenitors are obtained as 1.22±0.02M⊙ and 7.2±0.4⊙ respectively, suggesting that the upper mass limit of white dwarfs is less than 8M⊙. The final mass of white dwarfs shows no clear correlation with the initial mass of their progenitors, and it is found that a deficient gap of initial mass exists between ~4 and ~5.2M⊙. This gap seems to correspond to the mass range for carbon detonation or deflagration. The total expected numbers of white dwarfs are 11~22 in Hyades with 7 known white dwarfs and 17 in Praesepe with 8 known white dwarfs. These known white dwrfs are all younger than the others in both clusters. But one known white dwarf in Pleiades is older one among 2~3 expected white dwarfs.

본 논문에서는 이동물체에 의해 가진 받는 보의 동적반응을 보다 용이하게 다룰 수 있는 간결한 수치해석 알고리즘을 제안하였다. 구조물과 이동물체를 각각 균일한 Euler보와 질점으로 모델링하여 보의 운동방정식을 유도하였으며 이 식을 유연영향함수를 이용하여 적분형 미분방정식으로 바꾸어줌으로써 수치해석에 적용할 수 있는 형태로 바꾸어 주었다. 유도된 운동방정식을 모우드 해석기법을 이용하여 수치해를 구하였으며 기존의 수치해석 연구결과들과 비교하여 본 연구결과의 타당성을 검증함으로써 본 연구에서 개발한 수치해석 알고리즘은 이동물체에 의해 가진받는 보의 초기 해석과 설계과정에서 효율적으로 사용할 수 있음을 보였다.

In the best observed Pleiades cluster, the luminosity function(LF) and mass function(MF) for main sequence(MS) stars extended to Mv ≈ 15.5(V≈21) are very similar to the initial luminosity function(ILF) and initial mass function(IMF) for field stars in the solar neighborhood showing a bump at log m≃-0.05 and a dip at log m ≃ -0.12. This dip is equivalent to the Wielen dip appearing in the LF for the field stars. The occurence of these bump and dip is independent of adopted mass-luminosity relation(MLR) . and their characteristics could be explained by a time-dependent bimodal IMF. The model with this IMF gives a total cluster mass of ~700M⊙, ~25 brown dwarfs and ~3 white dwarfs if the upper mass limit of progenitor of white dwarf is greater than 4.5M⊙. The cluster age on the basis of LF for brightest stars is given by ~ 8×107yr and all stars in the cluster lie along the single age sequence in the C-M diagram without showing a large dispersion from the sequence.

We have reviewed three different techniques to estimate molecular cloud mass, and discussed the uncertainties involved. We found that determination of the most important parameter, the 13CO 13CO abundance, is not very sensitive to the real LTE conditions, and that any possible error in deriving LTE column density may not introduce an error in the total gas column density, as far as the visual extinction is established for the object cloud. The virial technique always endows the largest mass estimate as there are several uncertainties, even if the cloud is in virial equilibrium. The strong indicator of the cloud perturbation is the centroid velocity dispersion. The mass using CO luminosity is based on the empirical law, but weakly dependent on the virial assumption, thus it still gives a larger mass estimate. The mass discrepancy is likely to be inevitable, and a factor of two or three difference between mass estimates could easily be attributed to the uncertainties mentioned above. The LTE mass estimate may be the most reliable one if we use the relation visual extinction and 13CO 13CO column density of the object cloud, and the intercept is included.

We present two codes which estimates virial mass and LTE mass using IMFORT interface within IRAF (Image Reduction and Analysis Facility). It is discussed that threshold value (temperature or CO integrated intensity), which defines a reasonable cloud boundary and size, is the most important parameter determining accurate results. Several virial masses are to be obtained using the vir task, as well as three velocity dispersions including the centroid velocity dispersion, a turbulence indicator. LTE mass is to be estimated by using task lte as well as three by-product images. The 13CO 13CO abundance and threshold temperature of 13CO 13CO and 12CO 12CO peak temperatures are the most critical parameters in LTE technique.

Customary usage of oil at homes and rancidity of edible soybean oil by cooking frequency at homes and mass meal services were investigated. 80% of house wives bought the cooking oil by 1.8 f unit container and 70% of them read either the manufactured date or explanatory note for use. 85% of house wives kept oil in the storage case under sink or in the pantry chest, and 80% of oils were used once or twice and 20% used three times for cooking. Acid value(AV), iodine value(IV), peroxide value(POV), carbonyl value(CoV) and thiobarbituric acid value(TBAV) of fresh soybean oil were lower than standard level. In the rancidity by cooking frequency, the acid value, peroxide value, carbonyl value and thiobarbituric acid value increased significantly when oil was used once and iodine value decreased significantly when used once and twice at both mass meal services and homes. The level of the acid value, iodine value, carbonyl value and thiobarbituric acid value of oil used at mass meal services did not show significant difference from those of oil used at homes. But, the peroxide value of oil used thrice at mass meal services was significantly higher than those of homes.