• 천문학회보
• /
• 제44권1호
• /
• pp.68.3-68.3
• /
• 2019

Even though the initial mass function (IMF) of the first generation of stars played important roles in reionization of the universe, subsequent star formation, and chemical enrichment of the universe, it is still very uncertain. In this study, among the several indirect ways of estimating the IMF of the population III (Pop III) stars, we make use of extremely metal-poor (EMP; [Fe/H] < -3.0) stars in the Milky Way, in order to infer the characteristic mass range of Pop III stars. As the progenitors of many of the EMP stars are known to be Pop III stars, we attempt to construct the characteristic mass range of the progenitors (e.g., Pop III stars) of the EMP stares by comparing their observed abundance pattern of various chemical elements with chemical yields from supernova models.

• 천문학회보
• /
• 제43권2호
• /
• pp.52.2-52.2
• /
• 2018

The shape of a galaxy's spectral energy distribution ranging from ultraviolet (UV) to infrared (IR) wavelengths provides crucial information about the underlying stellar populations, metal contents, and star-formation history. Therefore, analysis of the SED is the main means through which astronomers study distant galaxies. However, interstellar dust absorbs and scatters UV and optical light, re-emitting the absorbed energy in the mid-IR and Far-IR. I present the updated 3D Monte-Carlo radaitive transfer code MoCafe to compute the radiative transfer of stellar, dust emission through a dusty medium. The code calculates the emission expected from dust not only in pure thermal equilibrium state but also in non-thermal equilibrium state. The stochastic heating of very small dust grains and/or PAHs is calculated by solving the transition probability matrix equation between different vibrational, internal energy states. The calculation of stochastic heating is computationally expensive. A pilot study of radiative transfer models of SEDs in clumpy (turbulent), galactic environments, which has been successfully used to understand the Calzetti attenuation curves in Seon & Draine (2016), is also presented.

• 천문학회보
• /
• 제43권2호
• /
• pp.55.1-55.1
• /
• 2018

Theoretical models of reionization require that approximately 10% of the Lyman Continumm (LyC) photons escape from their host dark matter haloes and re-ionize neutral hydrogen in the Universe. However, observations of Lyman break galaxies (LBGs) at z~3 report much lower escape fractions of $f_{esc}{\sim}1%$. In an attempt to understand the discrepancy, we perform radiation-hydrodynamics simulations of isolated disk galaxies using RAMSES-RT with high resolution (maximum ~ 9 pc). We find that $f_{esc}$ is ~6% on average for the reference run ($Z=0.1Z{\odot}$), whereas the fraction decreases to ~1% in the case of metal-rich disk ($Z=1Z{\odot}$). This happens because dense metal-poor gas clumps are disrupted early due to strong Lya pressure and supernova explosions, while star particles are trapped for a longer period of time in the metal-rich environments. We also find that $f_{esc}$ is still significant (~4%) even when the amount of metal-poor gas is increased by a factor of 5. Our preliminary results suggest that the low escape fractions in LBGs may be better explained by (locally) metal-enriched gas near young stars than high gas fractions in galaxies.

• 한국전산유체공학회지
• /
• 제21권2호
• /
• pp.70-80
• /
• 2016

The comparison of two commercial codes(FLUENT and STAR-CCM+) and an open-source code(OpenFOAM) are carried out for the aerodynamic analysis of flight vehicles at low speeds. Tailless blended-wing-body UCAV, main wing and propeller of HALE UAV(EAV-3) are chosen as geometries for the investigation. Using the same mesh, incompressible flow simulations are carried out and the results from three different codes are compared. In the linear region, the maximum difference of lift and drag coefficients of UCAV are found to be less than 2% and 5 counts, respectively and shows good agreement with wind tunnel test data. In a stall region, however, the reliability of RANS simulation is found to become poor and the uncertainty according to code also increases. The effect of turbulence models and meshes generated from different tools are also examined. The transition model yields better results in terms of drag which are much closer to the test data. The pitching moment is confirmed to be sensitive to the existence and the location of transition. For the case of EAV-3 wing, the difference of results with ${\kappa}-{\omega}$ SST model is increased when Reynolds number becomes low. The results for the propeller show good agreement within 1% difference of thrust. The reliability and uncertainty of three codes is found to be reasonable for the purpose of engineering use. However, the physical validity and reliability of results seem to be carefully examined when ${\kappa}-{\omega}$ SST model is used for aerodynamic simulation at low speeds or low Reynolds number conditions.

• 한국정보처리학회논문지
• /
• 제2권1호
• /
• pp.95-105
• /
• 1995

광전송에 의한 광통신 기술의 사용이 보편화 되면서 MAP 3.0규격은 광 파이버의 전송시 잡음 여유, 열악한 환경에서의 정상 동작, 안정성, 고속 전송의 장점 등으로 전송 매체로서 선택 사양에 규정하고 있다. 이러한 특성들은 제조 환경에서 광 네트워 크를 구축하는 것에 유용하다. 본 논문에서는 버스와 스타 구조의 사용을 포함한 광 패버 802.4의 MAP 네트워크 시스템 구축에 대하여 해석하고 광 패시브스타 네트워크와 FDDI 네트워크 모델을 제안 하였다. 그리고, MAP 규격의 물리 및 데이타 링크 계층 구 조에서 100 Mbps의 이중 링 구조의 FDDI 프로토콜을 제조 환경에서의 특성을 해석 하 였다. 또한 제조 환경에서 제안된 두 모델에 대하여 응용 서비스, 실시간 처리성, 토 폴로지면에서 비교하고 평가하였다.

• 천문학회지
• /
• 제29권1호
• /
• pp.63-73
• /
• 1996

The previous study of chemical evolution of the Galaxy is extended to the radial properties of the Galactic disk. The present model includes radial dependency of the time-dependent bimodal IMF, radial flow of material in the disk, and the change of type I supernova explosion rate with radial distance from the disk center as model parameters and observed gas and stellar density distributions and metallicity abundance gradient as observational constraints. The results of two models in this study explain the observed gas and stellar density distributions well, with the slope of the gas density gradient in the region of 4.5 kpc$Y_1$ and -0.123dex/kpc in model $Y_2$, respectively, which fit well the observed gradient of -0.l1dex/kpc. The abundance gradient reproduced in model $Y_1$ is getting flatter with decreasing radius, while that in model $Y_2$ is getting steeper, which fits better the observed abundance gradient. This result shows the necessity of exponentially increasing type I supernova explosion rate with decreasing radius in order to explain the observed abundance gradient in the disk. The fitness of observed density distribution and star formation rate distribution justifies the reliability of time-dependent bimodal IMF as a compound quantitative chemical evolution model of the Galaxy. The temporal variations of metallicity gradients for carbon, nitrogen and oxygen are also shown.

• 천문학회보
• /
• 제42권2호
• /
• pp.39.2-39.2
• /
• 2017

Over the last decade, deep studies of nearby galaxies have led to the discovery of vast stellar envelopes that are often rich in substructure. These components are naturally predicted in models of hierarchical galaxy assembly, and their observed properties place important constraints on the amount, nature, and history of satellite accretion. One of the most effective ways of mapping the peripheral regions of galaxies is through resolved star studies. Using wide-field cameras equipped to 8 m class telescopes, it has recently become possible to extend these studies to systems beyond the Local Group. Located at a distance of 3.6 Mpc, M81 is a prime target for wide-field mapping of its resolved stellar content. In this talk, we present the detailed results from our deep wide-field imaging survey of the M81 group with the Hyper Suprime-Cam (HSC), on the Subaru Telescope. We report on the analysis of the structures, stellar populations, and metallicities of old dwarf galaxies such as NGC3077, IKN, KDG061, as well as young stellar systems such as Arp's Loop and Holmberg IX. Several candidates for yet-undiscovered faint dwarf galaxies and young stellar clumps in the M81 group will also be introduced. The peculiar galaxy NGC3077 has been classified as the irregular galaxy. Okamoto et al. (2015, ApJ 809, L1) discovered an extended halo structure with S-shape elongated tails, obvious feature of tidal interaction. With a help of numerical simulation by Penarrubia et al. (2009, ApJ 698, 222), we will demonstrate that this tidal feature was formed during the latest close encounters between M81, M82, and NGC 3077, which induced star formation in tidally stripped gas far from the main bodies of galaxies. It is not clear whether the latest tidal interaction was the first close encounters of three galaxies. If NGC3077 is still surrounded by the dark matter halo, it implies that NGC3077 has undergone the first tidal stripping by larger companions. Kinematic studies of inter galactic globular clusters and planetary nebulae would tell us the past history of tidal interaction in this group of galaxies.

• 천문학회지
• /
• 제43권5호
• /
• pp.161-168
• /
• 2010

Magnetars are neutron stars possessing a magnetic field of about $10^{14}-10^{15}$ G at the surface. Thermodynamic properties of neutron star matter, approximated by pure neutron matter, are considered at finite temperature in strong magnetic fields up to $10^{18}$ G which could be relevant for the inner regions of magnetars. In the model with the Skyrme effective interaction, it is shown that a thermodynamically stable branch of solutions for the spin polarization parameter corresponds to the case when the majority of neutron spins are oriented opposite to the direction of the magnetic field (i.e. negative spin polarization). Moreover, starting from some threshold density, the self-consistent equations have also two other branches of solutions, corresponding to positive spin polarization. The influence of finite temperatures on spin polarization remains moderate in the Skyrme model up to temperatures relevant for protoneutron stars. In particular, the scenario with the metastable state characterized by positive spin polarization, considered at zero temperature in Phys. Rev. C 80, 065801 (2009), is preserved at finite temperatures as well. It is shown that, above certain density, the entropy for various branches of spin polarization in neutron matter with the Skyrme interaction in a strong magnetic field shows the unusual behavior, being larger than that of the nonpolarized state. By providing the corresponding low-temperature analysis, we prove that this unexpected behavior should be related to the dependence of the entropy of a spin polarized state on the effective masses of neutrons with spin up and spin down, and to a certain constraint on them which is violated in the respective density range.

• 해양환경안전학회지
• /
• 제22권7호
• /
• pp.876-883
• /
• 2016

본 연구에서는 카누 선체 재료를 탄소섬유복합재료로 선정하였으며, 선형설계는 선박 설계 상용프로그램인 SOLIDWORKS를 이용하여 수행하였다. 카누의 유동해석은 상용프로그램인 STAR-CCM+를 이용하여 자유수면의 파형을 살펴보고 수치해석 결과를 통하여 저항성능을 확인하였다. 그 결과, 흘수가 0.09 m일 경우에 4 m/s 미만의 선속으로, 흘수가 0.24 m인 경우에는 2 m/s 미만으로 운항하면 안전하다고 판단되며, 두 명의 성인이 속도를 내는 데에도 무리가 없음을 확인하였다. 또한, 해석결과를 적용하고 CFRP를 이용하여, 기존의 재료보다 20 % 가볍게 제작된 카누에 대해서도 간략히 소개하였다.

• 한국철도학회논문집
• /
• 제12권4호
• /
• pp.457-464
• /
• 2009

디젤 엔진 매연 필터의 입구부와 배출 가스 배출을 위한 배기관 연결을 직선 또는 곡선으로 형태로 연결하였을 때의 DPF 입구 유속 분포를 $STAR-CD^{(R)}$ 전산해석 프로그램을 사용하여 시뮬레이션하였다. 곡관의 형상을 나타내는 3 종류의 수치해석 용 격자 모델을 사용하여 DPF 입구에서의 유속 분포를 시뮬레이션 하였다. 피토관을 2차원 이송장치에 탑재하고 위치를 이동시키며 측정한 유속 분포와 동일한 조건에서 시뮬레이션한 결과와 비교하였다. DPF 입구와 $90^{\circ}$의 곡관이 연결된 조건에서 CFD 해석을 수행한 결과 입구 단면에서의 유속 분포가 말발굽 형태를 나타내었으며 최대 유속값이 DPF 중심축에서 약간 벗어난 위치에서 나타나고 있다. 이러한 CFD 해석결과는 실험 결과와 비교적 잘 일치하였다.