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McCoy 세포에서 Chlamydia trachomatis의 병원성 인자에 관한 연구
강정숙,최지영,차영주,김영주,김덕례,여명구,박열 조선대학교 생명과학연구소 1998 생명과학 연구 Vol.6 No.-
본 연구는 병원성 세균인 Chlamydia trachomatis(C. trachomatis)가 숙주세포에침습시 C. trachomatis의 병원성 인자와 C. trachomatis와 상호작용하는 숙주 세포막의 인자를 규명함으로써 숙주세포에 대한 감염율을 향상시켜 보다 향상된 진단 방법을 개발하기 위하여 수행하였다. C. trachomatis로 감염된 세포에서 기본소체의 막 단백질을 분리한 결과 각 혈청형의 39 kDa과 42 kDa에서 major outer membranes(MOMPs)이 관찰되었으며, 혈청형 E와 G의 MOMPs는 42.5 kDa으로 동일하였지만 혈청형 F, H, I, 그리고 K의 MOMPs는 각각 다르게 관찰되었다. C. trachomatis가 숙주세포로 침습시 관련된 병원성 인자에 대하여 조사하고자 단층세포로 배양된 배양용기에 C. trachomatis를 24, 48 그리고 73시간대별로 접종시켜 관찰한 결과 72시간의 MOMPs의 양이 가장 많이 증가하였으며 이 결과로 MOMPS이 C. trachomatis 병원성에 중요한 작용을 함을 확인할 수 있었다. C. trachomatis가 침습시 숙주세포의 막 단백질 변화양상을 관찰하기 위해 정상세포와 C. trachomatis로 1, 2, 3 그리고 4시간대별로 접종 시간을 달리한 숙주세포의 막 단백질을 분리한 결과 42 kDa의 단백질 양이 Chlamydia에 감염된 세포 내에서 증가됨을 관찰할 수 있었다. 이로 42 kDa의 막 단백질이 침습시 숙주세포 표면에 대한 수용체로서 작용함을 알 수 있었다. The present study was performed to analyze the pathogenic factors involved in the invasion process of Chlamydia trachomatis(C. trachomatis) into McCoy cells. In this study, elementary bodies(EBs) of C. trachomatis serotypes(E, F, G, H, I, K and LGV) could be isolated by the method of Percoll density gradient centrifugation and the pathogens of serotypes were also compared from whole-cell lysates by using sodium dodecyl sulfate-polyacrylamide gel elelectrophoresis. All chlamydial serotypes showed a single predominant protein ranging from 39 to 42 kDa. The major outer membrane proteins(MOMPs) of the E and G serotypes had an identical molecular weight of 42.5 kDa. In contrast, the MOMPs of the F, H, I and K serotypes were showed different molecular weights of MOMPs. By immunoblotting with anti-MOMP antibody it was revealed that the quantify of MOMPs was time-dependently increased when McCoy cells were infected with Chlamydia for 24, 48 and 72 hr. These results indicated that MOMPs are closely related to chlamydial infection into the host cell.
Relativistic Radiation Hydrodynamics for Accretion
Myeong-Gu Park 한국물리학회 2006 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.49 No.4
Accretion flow in general involves relativistic motions, radiative interaction, and strong gravity, all of which demand accurate relativistic treatment. I use the covariant tensor formalism to show how to derive the general radiation hydrodynamic equations for arbitrary coordinates or spacetimes. Frequency-integrated radiation moments defined in given tetrad frames are transformed to covariant forms. Interactions between radiation and matter are to be evaluated in the tetrad comoving with the gas while the hydrodynamic and radiation moment equations are written in covariant forms. This mixed-frame covariant approach is more straightforward to apply to accretion problems. The closure relation for inherently incomplete radiation moment equations is also discussed.#?
Relativistic Radiation Hydrodynamic Equations in Cylindrical Coordinates
Myeong-Gu Park 한국물리학회 2006 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.49 No.2I
In many astrophysical systems such as accretion disks and jets, radiation interacts with relativistically moving matter. With applications to such systems in mind, I use the covariant tensor conservation laws to derive special relativistic, time-dependent, three-dimensional energy and momentum equations for matter and radiation in cylindrical coordinates. The equations can be conveniently applied to various radiation hydrodynamic processes with cylindrical symmetry. Radiation moments, like the radiation energy density, flux, and pressure, are defined in the comoving (with the flow) frame first and then transformed to the corresponding covariant quantities. The interaction between matter and radiation is also described in the comoving frame while the equations are represented in coordinates that are fixed with respect to the central object. As a concrete example, the relativistic equations of motion for a cylindrical gas flow interacting with a spherically symmetric radiation field are presented.0002
STABILITY OF THE TWO-TEMPERATURE ACCRETION DISK
PARK MYEONG-GU The Korean Astronomical Society 1995 Journal of The Korean Astronomical Society Vol.28 No.1
The stability of the geometrically thin, two-temperature hot accretion disk is studied. The general criterion for thermal instability is derived from the linear local analyses, allowing for advective cooling and dynamics in the vertical direction. Specifically, classic unsaturated Comptonization disk is analysed in detail. We find five eigen-modes: (1) Heating mode grows in thermal time scale, $(5/3)({\alpha}{\omega})^{-1}$, where alpha is the viscosity parameter and w the Keplerian frequency. (2) Cooling mode decays in time scale, $(2/5)(T_e/T_i)({\alpha}{\omega})^{-1}$, where $T_e\;and\;T_i$ are the electron and ion temperatures, respectively. (3) Lightman-Eardley viscous mode decays in time scale, $(4/3)(\Lambda/H)^2({\alpha}{\omega})^{-1}$, where $\Lambda$ is the wavelength of the perturbation and H the unperturbed disk height. (4) Two vertically oscillating modes oscillate in Keplerian time scale, $(3/8)^{1/2}\omega^{-1}$ with growth rate $\propto\;(H/\Lambda)^2$. The inclusion of dynamics in the vertical direction does not affect the thermal instability, adding only the oscillatory modes which gradually grow for short wavelength modes. Also, the advective cooling is not strong enough to suppress the growth of heating modes, at least for geometrically thin disk. Non-linear development of the perturbation is followed for simple unsaturated Compton disk: depending on the initial proton temperature perturbation, the disk can evolve to decoupled state with hot protons and cool electrons, or to one-temperature state with very cool protons and electrons.