• Archives of Pharmacal Research
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• 제10권2호
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• pp.110-114
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• 1987

To correlate the conformational changes of DNA (Calf Thymus) with entrapment of DNA into liposomes, the effect of ions ($Na^+$, $Mg^{++}$on the entrapment of calf thymus DNA into liposomes was investigated. The effect of divalent ion ($Mg^{++}$ on the structural changes of DNA indicated by decrease of observed ellipticity at 274 nm and nonspecific binding of DNA to lipid bilayers was greater than monovalent ion ($\Na^+$). But the efficiency of DNA encapsulated was not altered. These results show that entrapment of DNA into liposomes is not due to nonspecific binding and structural changes because of electrostatic forces but to mechanical capture of DNA by the internal aqueous space of liposomes although divalent ion contributes large structural changes and more nonspecific association of DNA with liposomes due to strong charges.

• 천문학회지
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• 제2권1호
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• pp.1-9
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• 1969

On the instantaneous tidal relaxation approximation, formulae are derived for the ellipticities and virial theorem of a slightly flattened homogeneous rotating cluster (the largest axis of the cluster is directed towards the Galactic center), in terms of the Galactic tidal force and the characteristic intrinsic plus orbital angular velocity. The expression for a purely tidally-determined ellipticity is identical to that for an incompressible fluid body of uniform density. Orbital motion generally contributes significantly to the shape of the cluster. The virial theorem is identical to that for an isolated cluster except that the gravitational potential energy is multiplied by (1-${\chi}$), where ${\chi}$ is a positive tidal correction term. To obtain the actual mass of a cluster, the virial theorem mass based on an isolated cluster should be multiplied by the factor 1/(1-${\chi}$). The formulae are applied to open star clusters, the globular cluster ${\omega}$ Centauri, and dwarf elliptical galaxies in the Local Group.

• 천문학회지
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• 제35권3호
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• pp.123-130
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• 2002

An elliptical accretion disk may be formed by tidally disrupted debris of a flying-by star in an active galactic nucleus (AGN) or by tidal perturbation due to a companion in a binary black hole system. We investigate the iron K$\alpha$ line profiles expecting from a geometrically thin, relativistic, elliptical disk in terms of model parameters, and find that a broad and skewed line profile can be reproduced well. Its shape is variable to the model parameters, such as, the emissivity power-law index, the ellipticity of the disk, and the major axis orientation of the elliptical accretion disk. We suggest that our results may be useful to search for such an elliptical disk and consequently the tidal disruption event.

• 한국진공학회지
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• 제4권S2호
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• pp.24-29
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• 1995

The magnetic amd magneto-optical(MO)properties of Co-based multilayered(ML)films are known to vary sensitively according to the manufacturing methods and the film microstructures. Co/Pd and Co/Pt ML films with ultrathin layers of Co were prepared by alternating deposition in an ultrahigh-vacuum physical-vapor-deposition system. The individual layer thicknesses of the samples were estimated making use of the angular positions of x-ray diffraction peaks. The magnetic and MO properties were investigated, and correlated systematically to the structural parameters of the films. A Kerr spectrometer was self-manufactured to measure the MO properties such as Kerr rotation angle, ellipticity and reflectivity. The rms surface roughness was also measured using atomic force microscopy. Some of the samples showed good properties for MO medium, such as large perpendicular magnetic anisotropy and Kerr rotation, and perfect squareness of the magnetic hysteresis loop.

• 천문학회보
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• 제44권2호
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• pp.75.1-75.1
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• 2019

We introduce a novel method for reconstructing the projected dark matter mass maps of merging galaxy clusters by applying the convolutional neural network (CNN) to their weak lensing maps. We generate synthesized grayscale images from given weak lensing maps that preserve their averaged galaxy ellipticity. We then apply them to multi-layered CNN with architectures of alternating convolution and trans-convolution filters to predict the mass maps. We train our architecture with 1,000 Subaru/Suprime-Cam mock weak lensing maps, and our method have better mass map prediction than the Kaiser-Squires method with the following three aspects: (1) better pixel-to-pixel correlation, (2) more accurate finding of density peak position, and (3) free from mass-sheet degeneracy. We also apply our method to the HST weak lensing map of the El Gordo cluster and compare our result to the previous studies.

• Applied Biological Chemistry
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• 제46권4호
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• pp.305-310
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• 2003

Hydrophobic core가 변이된 유비퀴틴 단백질이 pH 2 용액에서 보이는 구조적인 특성을 여러 분광학적 방법으로 측정하였다. 낮은 pH값을 갖는 용액에서 이 변이 유비퀴틴의 intrinsic tryptophan fluorescence emission spectrum은 unfolded 상태보다 약간 blue shift되어 있고 또한 그 intensity도 상당히 낮게 나타났다. 이는 이 용액 조건에서 이 변이 유비퀴틴의 삼차구조가 약간 남아 있는 것을 의미한다. 같은 용액에서 이 변이 유비쥐틴의 far-UV circular dichroic spectrum은 native 상태나 unfolded 상태의 spectrum과 현저히 달랐으며 220 nm 에서의 molar ellipticity 값을 통하여 볼 때 pH 2인 용액에서 상당량의 이차구조를 지니고 있었다. 또한 같은 용액에서 이 변이 유비퀴틴은 hydrophobic dye인 8-anilinonaphthalene-1-sulfonic acid(ANS)외 fluorescence emission intensity를 증가시키고 fluorescence emission maximum이 짧은 파장에서 나타나게 하였다(blue shift). 이러한 현상은 pH 2 용액에서 이 변이 유비퀴틴의 hydrophobic core가 느슨하여져서 hydrophobic dye인 ANS가 결합할 수 있는 구조를 띠고 있음을 나타낸다. 이러한 분광학적인 관찰은 이 변이 유비귀틴이 pH 2인 용액에서 상당량의 이차구조를 지니고 있지만 hydrophobic core는 느슨하게 형성된 molten globule과 같은 형태를 지니고 있음을 나타낸다. 이 변이 유비퀴틴의 molten 히obule 형태는 단백질 폴딩 반응의 경로를 연구할 수 있는 좋은 모델이 될 수 있을 것으로 생각된다.

• Journal of Astronomy and Space Sciences
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• 제21권4호
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• pp.249-262
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• 2004

구상성단 NGC 6934의 밝은 거성 종족에 의한 중심부의 역학적 세부구조의 변화를 알아보기 위해서 NGC 6934의 BV 영상에 점광원 함수 측광과 표면측광을 실시하여, 성단 내 구성별들의 종족에 대한 성단 중심으로부터 타원률과 위치각의 변화를 얻었다. 타원률과 위치각의 전체적인 변화를 살펴보면 $r_{\eff}<3r_h$ 영역에서, 타원률은 $0.02{\sim}0.08$ 범위의 변화를 보이며, 위치각은 $-90^{\circ}{\sim}+90^{\circ}$ 범위에서 큰 변화 폭을 가지는 것으로 나타났다. 각 거성 종족의 제거에 따른 타원률과 위치각의 변화로부터, 성단의 $r_{\eff} 영역에서 가장 밝은 거성들(b-RGB)이 성단의 역학적 구조에 큰 영향을 미치고 있음을 알 수 있었다. 이 영역에서 b-RGB를 제외한 다른 거성 종족에 의한 타원률과 위치각의 변화는 밝은 거성 종족에 의한 변화에 비해 작게 나타났으며, 단, 위치각의 경우 어두운 거성(f-RGB)에 의한 역학적 세부구조 변화를 볼 수 있었다. $r_h영역에서는 수평계열 종족(RHB, BHB)과, f-RGB에 의한 $r_{eff}{\sim}60\;arcsec$ 근처의 타원률 및 위치각의 변화를 확인 하였다.

• 지구물리
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• 제3권1호
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• pp.37-48
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• 2000

다성분 복소 트레이스 분석법을 이용하여 지진에 의한 지면운동을 밝히고자 컴퓨터 합성 탄성파 자료와 자연 지진 자료를 대상으로 파선방향의 입자운동을 분석하였다. 합성 탄성파 자료에 적용시킨 결과, 실체파 합성 부분에서는 도달시각, 지속시간, 접근각 등을 정확히 찾을 수 있으며, 레일리파도 쉽게 인지된다. 규모 7.3의 심발 지진 자료로부터 입자운동의 분극특성을 계산한 결과, 종파의 수직성분과 수평성분의 순간위상차, 순간역타원율, 접근각은 각각 약 ${\pm}180^{\circ},\;0{\sim}0.25,\;-30^{\circ}{\sim}-45^{\circ}$의 값을 가지며, 이러한 분극특성으로부터 진원시간함수는 $6{\sim}7\;s$ 정도 지속되는 것으로 분석된다. 횡파의 경우는 순간위상차가 일정하지 않으며, $0{\sim}0.3$의 순간역타원율과 거의 수직의 접근각을 나타낸다. 횡파 도달 직전에 기록된 비교적 저주파의 신호는 분극특성으로부터 횡파와는 구별되는 종파의 일종으로 해석된다. 종파와 횡파의 도달시각을 이용하여 구한 속도와 파선변수는 각각 8.633 km/s, 4.762 km/s와 0.074 s/km, 0.197 s/km이며 동포와송비는 0.281로 계산된다.

• 천문학회보
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• 제39권2호
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• pp.70.1-70.1
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• 2014

We analyze a newly discovered galaxy-galaxy scale gravitational lens system, FLS 1718+59 in the Spitzer First Look Survey (FLS) field. A background galaxy (z = 0.245) is severely distorted by a foreground galaxy (z = 0.08), via gravitational lensing. We analyze this system by several methods, including surface brightness fitting (Galfit and Ellipse), gravitational lens modeling (gravlens), and spectral energy distribution fitting (Magphys). From Galfit and Ellipse we measure properties of the lens galaxy, such as the effective radius and the average surface brightness inside it, the ellipticity, and the position angle. gravlens gives us the total mass inside the Einstein radius ($R_{Ein}$), and Magphys provides us an estimate of the stellar mass inside $R_{Ein}$. By comparing these obtained parameters, we confirm that the lens galaxy is an elliptical galaxy on the Fundamental Plane, and calculate the stellar mass function inside $R_{Ein}$, and discuss the implications of the results regarding the initial mass function.

• 천문학회보
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• 제41권2호
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• pp.61.2-61.2
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• 2016

Nuclear rings at centers of barred galaxies exhibit strong star formation activities. They are thought to undergo gravitational instability when sufficiently massive. We approximate them as rigidly-rotating isothermal objects and investigate their gravitational instability. Using a self-consistent eld method, we first construct their equilibrium sequences specified by two parameters: ${\alpha}$ corresponding to the thermal energy relative to gravitational potential energy, and $R_B$ measuring the ellipticity or ring thickness. The density distributions in the meridional plane are steeper for smaller ${\alpha}$, and well approximated by those of infinite cylinders for slender rings. We also calculate the dispersion relations of nonaxisymmetric modes in rigidly-rotating slender rings with angular frequency ${\Omega}$ and central density ${\rho}_c$. Rings with smaller are found more unstable with a larger unstable range of the azimuthal mode number. The instability is completely suppressed by rotation when ${\Omega}$ exceeds the critical value. The critical angular frequency is found to be almost constant at $0.7(G{\rho}_c)^{1/2}$ for ${\alpha}$ > 0.01 and increases rapidly for smaller ${\alpha}$. We apply our results to a sample of observed star-forming rings and confirm that rings without a noticeable azimuthal age gradient of young star clusters are indeed gravitationally unstable.