Ambrosia beetle, Platypus koryoensis, is a vector of oak wilt disease caused by Raffaelea sp. in Korea. The degree of damage by oak wilt disease was dependent on the density of the beetles in the oak trunk, a relationship between the degree of damage by oak wilt disease and the density of beetle on the basis of the number of entry hole was studied. Entry hole distribution within tree trunk was analyzed by the nearest neighbor method. Thirty four oak trees (Quercus mongolica) located in survey area were selected and then degree of damage, the number of attack hole/623 ㎠ in upper (50 ㎝ from the surface) and lower (surface) trunk and the nearest neighbor distance between the holes were measured. The number of hole and the nearest neighbor distance in upper and lower part were positively correlated with each other. As the degree of damage was severer, the number of the holes increased, whereas the nearest neighbor distance decreased. The distribution pattern of the hole was changed from clumped one to uniform as the severity of damage increased. These results suggested that Platypus koryoensis attacked the oak tree in concentrative manner at initial stage of attack but at final stage, it distributed uniformly to reduce intraspecific competition between the beetles.

This study was performed to investigate the effect of laser-assisted hole in the zona pellucida (ZP) of frozen-thawed ICR mouse embryos on the process of hatching that is critical for expanded blastocysts to implant into endometrium, Vitrification medium, composed of ethylene glycol and sucrose supplemented with 7.5% (w/v) PVP, was used to freeze cell stage embryos recovered from oviducts of superovulated and mated female mice before storing them in . Right after thawing them, a laser beam was shot to make a hole in ZP followed by culturing in KSOM for and examining development to blastocyst and hatching every 12 hr. Laser-treated embryos showed significantly higher hatching rate compared to control (92.9% vs. 22.1%, p<0.05). From around Day 4, blastocysts developed from laser-treated embryos started hatching while the blastocysts of control group failed to hatch showing a lot of shrinkage. This study shows that a laser-assisted hole in ZP improves the hatching rate of blastocysts developed from frozen-thawed, in vitro cultured ICR mouse embryos.

The paper concerns an experimental and numerical study of fully developed laminar flow of a Newtonian, water and non-Newtonian fluids, 0.2% aqueous of sodium carboxymethyl cellulose(CMC) solution in concentric and eccentric annuli with combined bulk axial flow and inner cylinder rotation. Pressure losses and skin friction coefficients have been measured when the inner cylinder rotates at the speed of 0～300 rpm. The influences of rotation, radius ratio and working fluid on the annular flow field are investigated.

지반의 동적 변형 특성인 전단파 속도(V_s), 압축파 속도(V_p), 그리고 그에 따른 포아송 비(v)는 내진 설계나 내진 성능 평가 외에도 구조물의 거동 평가에 필요한 매우 중요한 지반 정수이다. 지난 수십 년 동안 이러한 지반 정수를 효율적이고 정밀하게 측정하기 위하여, 여러 가지 공내 탄성파 시험 기법들이 개발 및 적용되어 왔다. 본 연구에서는 가장 신뢰성이 높은 현장 탄성파 기법인 크로스홀 탄성파 시험을 지반 동적 물성 획득 기법으로 선정하였다. 지하수위 존재 여부에 관계 없이 토사뿐만 아니라 암반을 대상으로 크로스홀 시험을 성공적으로 수행할 수 있도록, 연직 시추공 안에서 지반을 대상으로 횡방향 가진이 가능한 스프링식 발진 장치를 개발하고, 두 곳의 기존 항만 부두 부지와 신규 LNG 저장 시설 두 부지로 구성된 국내 세 지역을 대상으로 크로스홀 탄성파 시험을 실시하였다. 대상 부지에서의 개발 발진 장치 적용을 통한 크로스홀 시험으로부터 지표 부근 토사부터 하부 공학적 기반암 및 지진학적 기반암으로 구성된 암반까지의 깊이별 V_s,\;V_p 및 v와 같은 지반 동적 특성을 매우 효율적으로 결정하였으며, 적용 대상 시설물인 기존 항만 부두 시설물의 내진 성능 평가 그리고 신규 LNG 저장 시설물의 내진 설계를 위한 근본 자료로 제시하였다.

The uniquely large dimensions of Giant radio galaxies (GRGs) make it possible to probe for stringent limits on total energy content, Faraday rotation, Alfven speeds, particle transport and radiation loss times. All of these quantities are more stringently limited or specified for GRG's than in more 'normal' FRII radio sources. I discuss how both global and detailed analyses of GRG's lead to constraints on the CR electron acceleration mechanisms in GRG's and by extension in all FRII radio sources. The properties of GRG's appear to rule out large scale Fermi-type shock acceleration. The plasma parameters in these systems set up conditions that are favorable for magnetic reconnection, or some other very efficient process of conversion of magnetic to particle energy. We conclude that whatever mechanism operates in GRG's is probably the primary extragalactic CR acceleration mechanism in the Universe.

지반의 횡파 속도 단면은 주로 다운흘 탄성파 탐사에 의존해 왔으나 최근에 MASW와 같은 표면파 탐사방법과 SCPT와 같은 탄성파 콘 관입시험법 등이 개발되어 사용되고 있다. 본 연구에서는 비고결 퇴적물에서 다운홀 탄성파 탐사, MASW, SCPT 등을 사용하여 횡파 속도 단면을 구하고 이들을 시추조사 결과와 비교하였다. 그 결과 퇴적물상의변화와 횡파 속도 변화는 밀접한 관계가 있음을 알 수 있었으며, 세 가지 횡파 속도 단면 중 SCPT가 퇴적물상의 변화에 가장 민감하게 반응하는 것을 알 수 있었다. SCPT 결과 퇴적층 내 약 8∼l2m 깊이에 주로 점토질 모래로 구성되어 있는 저속도 층이 있음을 알 수 있었다.

In the earlier papers we analyzed the axisymmetric, nonstationary electrodynamics of the central black hole and a surrounding thin accretion disk in an active galactic nucleus. Based on those papers we analyze the axisymmetric, nonstationary black hole magnetosphere in this paper. We concentrate on deriving the ‘Grad-Shafranov equations’; both in the force-free and non-force-free cases. In the time-independent limit our equations naturally coincide with stationary equations as they should.

In the earlier papers we analyzed the axisymmetric, nonstationary electrodynamics of the central black hole and a surrounding thin accretion disk in an active galactic nucleus. Based on those papers we analyze the axisymmetric, nonstationary force-free black hole magnetosphere and the motion of the plasma. We concentrate on deriving the totally new equations for the entropy incrrease and the angular momentum, energy extraction of the black hole.

Active galactic nuclei (AGNs) are distant, powerful sources of radiation over the entire electromagnetic spectrum, from radio waves to gamma-rays. There is much evidence that they are driven by gravitational accretion of stars, dust, and gas, onto central massive black holes (MBHs) imprisoning anywhere from $\~$ 수식 이미지1 to $\~$ 수식 이미지10,000 million solar masses; such objects may naturally form in the centers of galaxies during their normal dynamical evolution. A small fraction of AGNs, of the radio-loud type (RLAGNs), are somehow able to generate powerful synchrotron-emitting structures (cores, jets, lobes) with sizes ranging from pc to Mpc. A brief summary of AGN observations and theories is given, with an emphasis on RLAGNs. Preliminary results from the imaging of 10000 extragalactic radio sources observed in the MITVLA snapshot survey, and from a new analytic theory of the time-variable power output from Kerr black hole magnetospheres, are presented. To better understand the complex physical processes within the central engines of AGNs, it is important to confront the observations with theories, from the viewpoint of analyzing the time-variable behaviours of AGNs - which have been recorded over both 'short' human (10 0-10 9s) and 'long' cosmic (10 13 - 10 17 s) timescales. Some key ingredients of a basic mathematical formalism are outlined, which may help in building detailed Monte-Carlo models of evolving AGN populations; such numerical calculations should be potentially important tools for useful interpretation of the large amounts of statistical data now publicly available for both AGNs and RLAGNs.

승용차의 휠은 타이어와 차체 무게를 지지하며, 회전력과 정지력을 노면으로 전달한다. 휠의 경량화는 차량의 연료효율에 효과적이므로, 스틸휠이 무게를 최소화하도록 디스크 홀이 형상을 최적화 하였다. 설계모델은 Pro/ENGINEER를 사용하여 설정하고, 설계모델의 해석은 ANSYS를 이용하였다. 범용 소프트웨어간의 직접적인 자료의 전달이 어려우므로 두 프로그램을 병합 사용하기 위해, 반응표면법을 이용한 근사함수를 구하였다. 5수준의 요인배치법의 실험값을 사용하여 최대응력과 최대 변위를 추출하였다. 초기 모델은 14인치 승용차용 스틸휠을 사용하였고, 디스크 홀의 폭을 설계변수로 선택하였다. 순차이차계획법과 활성화제약조건을 사용하는 PLBA(Pahenichny-Lim-Belegundu-Arora) 알고르즘을 이용하여 최적해를 구하였다.

In the earlier papers we analyzed the axisymmetric, nonstationary electrodynamics of the central black hole and a surrounding thin accretion disk in an active galactic nucleus. Based on those papers we analyze the axisymmetric, nonstationary force-free black hole magnetosphere and the motion of the plasma. We concentrate on deriving the relations between the velocity components of the plasma and those of the accreting magnetic field lines. We conclude that the former are given by the sum of the latter and the magnetic field terms.