In the previous work we made a long term evolution code for the central black hole in an active galactic nucleus under the assumption that the Blandford-Znajek process is the source of the emission. Using our code we get the evolution of the angular velocity of the precession for a supermassive black hole. We consider a hole at the center of an axisymmetric, ellipsoidal galactic nucleus. Our numerical results show that, only for the cases such that the stellar density or the mass of the black hole is large enough, the precession of the black hole - presumably the precession of the galactic jet - is interestingly large.

We investigate the dynamical evolution of globular clusters under the diffusion, the Galactic tide, and the presence of halo black holes. We compare the results with our previous work which considers the diffusion processes and the Galactic tide. We find the followings: (1) The black holes contribute the expansion of the outer part of the cluster. (2) There is no evidence for dependence on the orbital phase of the cluster as in our previous work. (3) The models of linear and Gaussian velocity distribution for the halo black holes do not show any significant differences in all cases. (4) The perturbation of black holes reduces the number of stars in lower energy regions. (5) There is a significant number of stars with retrograde orbits beyond the cutoff radius especially in the case of diffusion and the perturbation of black holes.

Recent spectroscopic observations indicate concentration of dark masses in the nuclei of nearby galaxies. This has been usually interpreted as the presence of massive black holes in these nuclei. Alternative explanations such as the dark cluster composed of low mass stars (brown dwarfs) or dark stellar remnants are possible provided that these systems can be stably maintained for the age of galaxies. For the case of low mass star cluster, mass of individual stars can grow to that of conventional stars in collision time scale. The requirement of collision time scale being shorter than the Hubble time gives the minimum cluster size. For typical conditions of M31 or M32, the half-mass radii of dark clusters can be as small as 0.1 arcsecond. For the case of clusters composed of stellar remnants, core-collapse and post-collapse expansion are required to take place in longer than Hubble time. Simple estimates reveal that the size of these clusters also can be small enough that no contradiction with observational data exists for the clusters made of white dwarfs or neutron stars. We then considered the possible outcomes of interactions between the black hole and the surrounding stellar system. Under typical conditions of M31 or M32, tidal disruption will occur every 103 103 to 104 104 years. We present a simple scenario for the evolution of stellar debris based on basic principles. While the accretion of stellar material could produce large amount of radiation so that the mass-to-light ratio can become too small compared to observational values it is too early to rule out the black hole model because the black hole can consume most of the stellar debris in time scale much shorter than mean time between two successive tidal disruptions. Finally we outline recent effort to simulate the process of tidal disruption and subsequent evolution of the stellar debris numerically using Smoothed Particle Hydrodynamics technique.

Energy density evolution of primordial black holes(PBHs) due to quantum gravitational tunneling effect in the very early Universe is calculated for the four cases of GUTs(grand unified theories) (SM, SUSY SM, SUSY SU(5), SU(5)). For the three of them (SM, SUSY SM, SUSY SU(5)), it is confirmed that there are a considerable amount of PBHs and so it may give a firm support to Lindley's paper(1981) in which he tried to solve the baryon asymmetry problem. It is shown that the formation of PBHs increases the cosmic scale factor R and decreases the total energy density ρt ρt faster than in the usual radiation dominated era.

고력볼트의 현장 조립시 볼트 구멍 간의 불일치로 인하여 볼트 구멍을 확장하는 경우가 빈번하게 발생하고 있으며, 이를 위해서 외국 기준에서는 볼트 구멍 크기, 형태, 하중 방향에 따라 미끄럼하중에 대한 규정을 따로 두고 있다. 그러나 우리나라의 경우 과대구멍에 대한 시방규정이나 이에 대한 접합부 특성에 관한 연구는 미흡한 실정이다. 따라서, 접합부재 표면처리와 볼트구멍 크기의 변화가 접합부 내력에 어떠한 영향을 미치는 지를 실험을 통해 정량적으로 평가할 필요가 있다. 본 연구에서는 볼트 구멍 크기 및 형태에 따른 접합부의 미끄럼하중의 변화와 체결 후, 장기축력이완의 경향을 분석하기 위하여 160시간 및 800시간 동안 고력볼트의 축력의 변화를 측정하였다. 본 실험대상 고력볼트로 KS B 2819에 규정된 TS(Torque Shear)형 고력볼트를 사용하였다. 표준 볼트구멍 대비 그 외 볼트구멍의 미끄럼하중의 변화는 10% 미만으로 나타났으며, 장기축력이완은 직경 2.5배의 슬롯구멍에서, 2.66%로 가장 높게 나타났다.

The effects of modified atmosphere(MA) storage for fresh red chili pepper and red bell pepper fruits were investigated with storing in polyethylene film with various fine holes. During the storage of the both pepper fruits, the weight loss, color change, mold emergence, and firmness were evaluated. The weight loss of pepper fruits packaged without holes on film was less than 3%, even though it was each 50% and 25% for non packaged red chili pepper and red bell pepper fruits. The rates of mold emergence of red chili pepper and red bell pepper fruits were reached to each 60% and 50% at the end of storage period as stored in film without holes. However, the rate of mold emergence of pepper fruits was lowered when fruits were stored in MA with low relative humidity (70∼80%). The color and firmness of pepper fruits were not much changed when fruits were stored in MA with high humidity.