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.

Dextran(Mw.:500,000)용액의 한외여과에 있어서, 현재 나권형 모듈의 유로형성체로 사용되는 난류촉진물체를 적용하여 실험한 결과, 난류촉진물체의 mesh가 증가할수록 막투과 flux가 향상되었으며, 난류영역에서는 층류영역에 비해 순환유속과 난류촉진물체의 사용에 따른 막투과 flux에 대한 영향이 상대적으로 적었다. 난류촉진물체의 사용에 따른 막투과 flux 향상율은 사용한 membrane의 종류에 따라 층류영역의 경우 최대 112%, 난류영역의 경우 50%에 달하였다. 또한 난류촉진물체를 사용함으로써 한외여과막의 고분자 용질에 대한 배제 성능을 높일 수 있었으며, 이러한 flux 및 배제 성능 증가 등의 효과들은 높은 조작압력차와 낮은 순환유속(농도분극이 상대적으로 심한 영역)에서 더욱 두드러졌다. 그러나, 난류촉진물체의 mesh 수와 순환유속이 증가함에 따라 한외여과 cell 내에서의 압력손실도 증가하였으며, 특히 난류영역에서는 그 영향이 매우 심하였으므로 실제 공정 설계시 순환유속과 압력차 및 난류촉진물체 형태에 따른 압력손실을 반드시 고려해 주어야 함을 알 수 있었다. 물질전달계수 예측을 위한 기존의 물질전달 상관관계식을 농도분극층에서의 고분자 물질의 물성변화를 고려하고 경계층 저항 모델에 근거하여 보정하였는 바, 기존의 관계식에 비해 오차를 줄일 수 있었으며, 이때의 관계식은 다음과 같았다.Nsh}=0.151(NRe})0.199}(NSc})0.22}(NScm})0.197};(625

본 실험은 시설오이의 상품성 향상 및 생산성 증대를 위하여 주지형인 만능청장마디오이와 측지형인 사엽오이를 유인방법을 달리하여 재배하였으며 그 결과는 다음과 같다. 1. 유인방법 개선을 위한 오이의 저절위 착과특성을 조사하였던 바, 만능청장마디오이의 경우는 3마디까지, 사엽오이의 경우는 4마디까지가 수량 및 상품성이 불량하여 적과재배하는 것이 효과적이었다. 2. 오이의 유인방법 별 초기생육 및 과실의 개화시 자방중, 곡과도, 생장해석면에서 만능청장마디 오이는 횡유인, 종유인, 사면유인 순으로 좋았고 사엽오이는 횡유인, 사면유인, 종유인 순으로 좋게 나타났다. 3. 오이의 유인방법에 따라 초고별 상대조도와 적산엽면적지수로 본 작물의 수광태세는 만능청장 마디오이에서는 종유인과 횡유인이 사면유인보다 양호하였고 사엽오이는 횡유인, 종유인, 사면유인 순으로 나타났다. 4. 수량 및 품질은 만능청장마디오이와 사엽오이 모두에게 횡유인이 가장 우수하게 나타났다.

This study was undertaken to investigate the relationship between body mass index and the food habits of college students. For this purpose, 1030 students of Seoul National University were asked to fill out the questionnaires for the food habit and weight control. Actual weights were also measured, on the spot. The results obtained were as follows. 1. Average height and weight were 173.15 cm, 63.83 kg for male, and 160.52 cm, 52.73 kg for females. The prevalence of underweight, normal and overweight was 32.3, 61.7, 5.5%, respectively. 2. Food habit scores of obese females were lower than normal or underweight females. Male subjects did not show significantly different scores among three groups. 3. Female obese subjects have lower scores than the other groups on the balanced intake of five basic food groups and on the regular meal intakes. Male obese subjects have cholesterol-rich food and animal fat more frequently than normal and underweight males. Male underweight subjects have lower food habit scores on the balanced intake of five basic food groups. 4. Males want to gain weight slightly and females want to lose 4.65 kg weight. All females want to lose weights. Obese males and females want to lose 10 kg weights.

The sample of sub dwarfs are selected from LHS catalogue on the bases of the reduced proper motion diagram utilizing Chui criteria, and confirmed with the available photometric and/or kinematic data. Among them, 20 sub dwarfs have trigonometric parallaxes with accuracy better than 20 % . The color­absolute magnitude relation is derived with them. By adopting this color-magnitude relation and V / V m method, we have derived the sub dwarf luminosity function over the absolute magnitude range of M v = 4.5 and 9.5. This halo luminosity function is consistent with that of Eggen(1987). By adopting the available mass-luminosity relations for halo stars, we have found that the halo IMF is steeper than disk IMFs of Scalo(1986) and Salpter(1955) in this small mass region.