We have conducted VI CCD photometry of the open cluster NGC 6819 in order to understand the effects of dynamical evolution in old open clusters. Our photometry covers 18'× 18' on the sky, centered on the cluster, which seems to cover the whole cluster field. Our photometry reaches down to V ≈ 20.5, which allows us to analyze the luminosity function and spatial distribution of stars brighter than Mv ≈ 8.5. There is a clear evidence for mass segregation in NGC 6819, i.e., the giants and upper main-sequence stars are concentrated in the inner regions, whereas the lower main-sequence stars distribute almost uniformly throughout the cluster. The luminosity function of the main-sequence stars of NGC 6819 is almost flat. The flat luminosity function indicates that a large number of low mass stars has escaped from the cluster unless its initial mass function is much different from the Salpeter type (Φ(m)∝ m-(1+x),x = 1.35).

We have conducted UBVI CCD photometry of an intermediate-age open cluster NGC 559 to investigate the effect of dynamical evolution on the stellar distributions in NGC 559. Our photometry allows better estimates of distance and age of the cluster owing to much deeper photometry (V ≤ 21) than previous ones. It is found that the luminosity function and mass function as well as the spatial stellar distributions are affected by the dynamical evolution. Mass segregation leads to the central concentration of the high mass stars, which results in the flattened mass function inside the half mass radius.

We present UBVI CCD photometry of the stellar contents and globular cluster(GC) candidates in the spiral galaxy NGC 300 in the Sculptor group. Color-magnitude diagrams for 18 OB associations having more than 30 member stars are presented. The slope of the initial mass function for the bright stars in NGC 300 is estimated to be Γ = -2.6 ± 0.3. Assuming the distance to NGC 300 of (m - M)o = 26.53 ± 0.07, the mean absolute magnitude of three brightest blue stars is obtained to be < MvBSG (3) > = -8.95 mag. We have performed search for GCs in NGC 300 and have found 17 GC candidates in this galaxy. Some characteristics of these GC candidates are discussed.

UBV RI and Hα photometry has been performed for the open cluster NGC 6531. A total of 56 bright main sequence (MS) members were selected from their positions in photometric diagrams. We also classified 7 pre-main sequence (PMS) stars and 6 PMS candidates with Hα emission from Hα photometry. We determined a reddening of < E(B - V) >= 0.29 ± 0.03 and a distance modulus of Vo - Mv = 10.5 for the cluster. From the comparison of our photometric results to theoretical evolution models, we derived a MS turnoff age of 7.5 Myr and a PMS age spread of ~4 Myr. The IMF slope Γ, calculated in the mass range of 0.45 ≤ log m ≤ 1.35 is a steep value of Γ = -1.8 ±0.6.

UBVI CCD photometry of open cluster NGC 2324 is presented. C-M diagrams of this cluster show well-defined main sequence with a red giant clump centered at B - V =1.05, V =13.45. We derived the major cluster characteristics; E(B - V)=0.17±0.12 from color-color diagram and mean color of red giant clump stars, (m - M)o=13.1±0.1 from zero age main sequence fitting, and [Fe/H]~-0.32 from comparison the theoretical model developed by Bertelli et al. (1994) to the observed C-M diagrams. We estimate the age of NGC 2324 to be log t~8.8 by applying isochrone fitting and morphological age index method.

본 논문에서는 클러스터 시스템을 이용하여 프리스트레스트 콘크리트 프레임의 병렬 비선형해석이 가능한 해석수단을 제시하였다. Win 98 및 Linux 운영체제 하의 PC 및 Ethernet을 활용하여 저가의 클러스터 시스템을 구축하였고 메시지 전송을 위하여 MPI를 사용하였다. 비선형해석에 있어 해석시간의 대부분을 차지하는 반복계산과정 중 병렬계산에 의한 효율이 높은 접선강도매트릭스의 형성 및 요소응력계산, 재료상태 결정, 부재파괴 검토, 불평형하중 계산과정에 대한 병렬계산 알고리즘을 메시지 전송방식을 이용하여 제시하고 클러스터 시스템 상에서 구현했다. 캔틸레버 보와 PSC 거더교를 대상으로 클러스터 컴퓨팅을 이용한 비 선형해석을 수행한 결과 노트가 4개일 경우의 성능향상은 고려한 비선형형성 및 문제의 크기에 따라 다르나 Win98 환경에서 최소 2.46배에서 최대 3.18배로 나타났고 Linux 환경에서 최소 3.16배에서 최대 3.74배로 나타났으며 통신환경의 개선에 따라 증대될 것으로 기대된다.

A centrifugally atomized 2024A1/SiC/sub p/ composites were extruded to study effect of clusters on mechanical properties, and a model was proposed that the strength of MMCs would be estimated from the load transfer model approach that taken into consideration of the clusters. This model has been successfully utilized to predict the strength and fracture toughness of MMCs. The experimental and calculated results show coincidence and that the fracture toughness decreases with increasing the volume fraction of particles. On the basis of experimental observations, we suggest that the strength and fracture toughness of particle reinforced MMCs may be calculated from; σ/sub y/=σ/sub m/V/sub m/+σ/sub r/(V/sub r/-V/sub c)-σ/sub r/V/sub c/, K/sub IQ/=σ/sub Y/((3πt)((r/sub r//V/sub r/)(r/sub c//V/sub c/))/sup 1/2/)/sup 1/2/, respectively.

We present the results of near-IR band (JHK) photometric study for the old open cluster To 2. Combined with existing optical data, our IR photometry is used to derive the reddening E(B- V)=0.24±0.12 and the distance (m-M)o=14.6±0.42. Comparison with theoretical isochrones suggests the age and metallicity of To 2 are log t~9.3 and [Fe/H]~-0.3, respectively.

CN and CH band strengths for ten new bright giants in the globular cluster M15 have been measured from archival spectra obtained with the Multiple Mirror Telescope. Using published indices for other bright M15 giants, a CN-CH band strength anticorrelation is found for bright red giants. However, stars that do not follow the CN-CH anticorrelation are also found. They seem to show a positive correlation between the two indices. Among them, all the AGB and HB stars of the sample are included. Stars I-38 and X6, which are located near the RGB fiducial line in the CMD, have low measured CH(G) indices compared with other RGB stars. Stars IV-38, S4, and S1, which are all near the RGB tip, have strong measured CH(G) indices. Therefore, most of their evolutionary states are suspected to be different from those of a normal single RGB star.

Many models of globular cluster formation assume the presence of cold dense clouds in early universe. Here we re-examine the Fall & Rees (1985) model for formation of proto-globular cluster clouds (PGCCs) via thermal instabilities in a protogalactic halo. We first argue, based on the previous study of two-dimensional numerical simulations of thermally unstable clouds in a stratified halo of galaxy clusters by Real et al. (1991), that under the protogalactic environments only nonlinear (δ≳1) density inhomogeneities can condense into PGCCs without being disrupted by the buoyancy-driven dynamical instabilities. We then carry out numerical simulations of the collapse of overdense douds in one-dimensional spherical geometry, including self-gravity and radiative cooling down to T = 10 4 K. Since imprinting of Jeans mass at 10 4 K is essential to this model, here we focus on the cases where external UV background radiation prevents the formation of H2 molecules and so prevent the cloud from cooling below 10 4 K. The quantitative results from these simulations can be summarized as follows: 1) Perturbations smaller than Mmin ~(10 5.6 M⊙)(nh/0.05cm-3)-2 cool isobarically, where nh is the unperturbed halo density, while perturbations larger than Mmax ~(10 8 M⊙)(nh/0.05 cm-3)-2 cool isochorically and thermal instabilities do not operate. On the other hand, intermediate size perturbations (Mmin < Mpgcc < Mmax) are compressed supersonically, accompanied by strong accretion shocks. 2) For supersonically collapsing clouds, the density compression factor after they cool to Tc = 10 4 K range 10 2.5 - 10 6, while the isobaric compression factor is only 10 2.5. 3) Isobarically collapsed clouds (M < Mmin) are too small to be gravitationally bound. For supersonically collapsing clouds, however, the Jeans mass can be reduced to as small as 10 5.5 M⊙(nh/0.05 cm-3)-1/2 at the maximum compression owing to the increased density compression. 4) The density profile of simulated PGCCs can be approximated by a constant core with a halo of p∝ r-2 rather than a singular isothermal sphere.