• 지구물리와물리탐사
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• 제27권1호
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• pp.51-56
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• 2024

논문에서는 타원판의 벡터 중력과 중력 변화율 텐서 반응식을 유도하였다. 타원판의 벡터 중력은 이중 적분으로 표현한 타원판에 의한 중력 퍼텐셜을 각 축 방향으로 미분하여 유도한다. 이중 적분으로 정의된 타원판에 의한 벡터 중력은 복소 그린 정리를 이용하여 타원판 경계를 따라 폐곡선의 선적분으로 변형한다. 최종적으로 타원판 경계를 매개변수로 설정하여 1차원 수치적분을 통하여 타원판에 의한 벡터 중력을 유도한다. 타원판에 의한 중력 변화율 텐서의 xz, yz, zz성분은 타원판의 벡터 중력을 수직 방향으로 미분하여 구한다. xx, yy, xy성분은 이중 적분 형태의 벡터 중력의 수평 성분을 먼저 수평 방향으로 미분한 후 복소 그린 정리를 이용하여 유도한다.

• 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.

• 지구물리와물리탐사
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• 제27권2호
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• pp.108-118
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• 2024

이 논문에서는 타원판의 자력과 자력 변화율 텐서 반응식을 유도하였다. 화성암 관입이나 킴벌라이트 구조 등은 축 대칭성을 가지면서 단면이 타원인 경우가 많다. 타원 단면의 넓이가 변하는 타원 기둥은 타원판의 조합으로 모사할 수 있다. 타원판의 자력 반응은 이전 논문(Rim, 2024)에서 유도한 중력 변화율 텐서에 자화 방향에 대한 정보를 포함시킨 포아송 관계식을 이용하여 유도하였다. 타원판의 자력 변화율 텐서는 벡터 자력을 미분하여 유도하는데 타원판의 인력 퍼텐셜을 각 축방향으로 3회 미분한 총 10개의 삼중 미분 함수를 구하는 것과 동일하다. 미분의 순서는 바꾸는 것이 가능하므로 결과적으로 자력 변화율 텐서는 타원판의 인력 퍼텐셜을 3회 미분한 후, 복소 평면에서 타원판의 경계를 폐곡선으로 하는 경로를 따라 선적분으로 변환하여 유도된다. 이 논문에서 복소 평면에서 선적분으로 유도한 자력 및 자력 변화율 텐서 반응식은 립쉬츠-한켈 적분으로 유도한 원판의 자력 및 자력 변화율 텐서 반응식과 완벽하게 일치함을 보였다.

• 천문학회보
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• 제43권1호
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• pp.32.2-32.2
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• 2018

We present the structural parameters of ~ 910 dwarf elliptical-like galaxies in the local universe ($z{\lesssim}0.01$) derived from the r-band images of the Sloan Digital SKy Survey (SDSS). We examine the dependence of structural parameters on the morphological types (dS0, dE, dEbc, dSph, and dEblue) and the environment. There is not much difference in the structural parameters among the five subtypes but the mean surface brightness within the effective radius (<${\mu}e$>) of dSph galaxies is clearly different from that of other subtypes. The frequency of disk features such as spiral arm, bar, lens, and rings strongly depends on the morphology of dwarf elliptical-like galaxies with no disk features in dSph galaxies. The absence of disk features and the low surface brightness of dSph galaxies are thought to be closely related to their low mass which leads to different evolution from other subtypes of dwarf elliptical-like galaxies. Density Environments Using IMSNG.

• 한국윤활학회:학술대회논문집
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• 한국윤활학회 2003년도 학술대회지
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• pp.348-354
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• 2003

An analysis of the dynamic behavior between disk and roller has been performed when the torque is transmitted to toroidal IVT (Infinitely Variable Transmission). The contact area, shape and pressure with elliptical shapes between disk and roller are computed as the transmission ratios are changed. This study will give the information of contact shapes between roller-input dist and roller-output disk which are working under the most severe condition. The computed results are expected to guide the design criteria for the enhanced endurance li(e. Furthermore, the investigation of contact behaviors is very crucial to develop the traction oil that the efficiency of IVT system is most dependent on.

• 한국정밀공학회:학술대회논문집
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• 한국정밀공학회 2012년도 춘계학술대회 논문집
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• pp.957-958
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• 2012

• 천문학회보
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• 제42권2호
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• pp.46.2-46.2
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• 2017

We will present a discovery of an elliptical jellyfish galaxy in Abell 2670 (Sheen et al. 2017, ApJL, 840, L7). Our MUSE IFU spectra revealed a rotating gas disk in the center of the galaxy and long ionised gas tails emanating from the disk. Its one-sided tails and a tadpole-like morphology of star-forming blobs around the galaxy suggested that the galaxy is experiencing strong ram-pressure stripping in the cluster environment. Stellar kinematics with stellar absorption lines in the MUSE spectra demonstrated that the galaxy is an elliptical galaxy without any hint of a stellar disk. Then, the primary question would be the origin of the rich gas component in the elliptical galaxy. A plausible scenario is a wet merger with a gas-rich companion. In order to investigate star formation history of the system (the galaxy and star-forming blobs), we derived star-formation rate and metallicity from the MUSE spectra. Photometric UV-Optica-IR SED fitting was also performed using GALEX, SDSS, 2MASS and WISE data, to estimate dust and gas masses in the system. For a better understanding of star formation history and environmental effect of this galaxy, FIR/sub-mm follow-up observations are proposed.

• 한국광학회:학술대회논문집
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• 한국광학회 1989년도 제4회 파동 및 레이저 학술발표회 4th Conference on Waves and lasers 논문집 - 한국광학회
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• pp.26-31
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• 1989

Optical working machines are developed. the machines are to be used in the preparation of Nd-phosphate glass amplifier rod and elliptical disk amplifier plate of the high power Nd-YLF-phosphate glass laser amplifier system. In this report, the working principles of the machines are presented, and several results are shown by photographes, design drawing and the disks actually fabricated by using the machines.

• 천문학회보
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• 제44권1호
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• pp.38.2-38.2
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• 2019

S0 galaxies are mostly known to be formed in dense environments from spiral progenitors. Recently, however, a new formation scenario has been suggested that field S0s can be formed from elliptical progenitors. The Sombrero galaxy (M104, NGC 4594) is a massive disk galaxy located in the field environment, and its morphological type has been controversial from Sa to E. Thus, it is an ideal target to test the new scenario. We trace the giant halo of M104 with globular clusters to test this scenario. From the wide images obtained with CFHT/MegaCam, we find a large number of globular clusters in this galaxy. We also confirm their membership by measuring the radial velocities from the spectra obtained with MMT/Hectospec. The color distribution of these globular clusters is bimodal, and blue (metal-poor) globular clusters are more spatially widely spread than red (metal-rich) globular clusters. This indicates that M104 hosts a giant metal-poor halo as well as an inner metal-rich halo. Combining this result with the fact that M104 is unusually massive and brighter than other spiral galaxies, we infer that M104 was indeed a massive elliptical galaxy that had formed a metal-rich halo by gas-rich mergers and a metal-poor halo by gas-poor mergers. In addition, we find young star clusters around the disk of M104, which shows that the disk formed after the spheroidal halos had formed. In conclusion, we suggest that M104 was originally a massive elliptical galaxy and was transformed to a lenticular galaxy by acquiring its disk later.

• 천문학회보
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• 제41권1호
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• pp.39.3-39.3
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• 2016

About one tenth of dwarf elliptical galaxies found in the Virgo cluster have a disk component, and some of them even possess substructures such as bars, lens, and spiral arms. We use N-body simulations to study the formation of these non-axisymmetric features in disky dwarf elliptical galaxies. By mimicking VCC 856, a bulgeless dwarf galaxy with embedded faint spiral arms, we construct 11 sets of initial conditions with slight dynamical variations based on observational data. Our standard model starts slowly to form a bar at ~3 Gyr and then undergoes buckling instability that temporarily weakens the bar although the bar strength continues to grow afterward. We find 9 of our models are unstable to bar formation and undergo buckling instability. This suggests that disky dwarf elliptical galaxies are intrinsically unstable to form bars, accounting for a population of barred dwarf galaxies in the outskirts of the Virgo cluster. To understand the origin of the faint grand-design spiral arms, we additionally construct 6 sets of models that undergo tidal interactions with their neighbors. We find that faint spiral arms consistent with observations develop when tidal forcing is relatively weak although strong encounter still results in bar formation. We discuss our results in light of the dynamical evolution of dwarf elliptical galaxies including mergers.