• 천문학회보
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• 제41권1호
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• pp.68.1-68.1
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• 2016

Binary black hole mergers are one of the important candidate of gravitational wave (GW) emission. Recently a successful GW observation was done by LIGO team, but it is still uncertain how many GW signals will be observable. In this research, we perform simplified N-body simulations containing three mass components, ordinary stars with two kind of stellar mass black holes. Various BH compositions are tested to investigate the effect of BH mass function on binary formation rate. As a result, we find the binary formation rate is not much affected by BH mass function and always around 30 %, but the detectable merging binaries are largely depend on higher mass BH population.

• Asian Journal of Atmospheric Environment
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• 제10권1호
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• pp.1-12
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• 2016

Numerous researchers have proposed that surface area is a more appropriate indicator than mass for evaluating pulmonary inflammatory responses caused by exposure to fine and ultrafine particles. In this study, measurements of surface area concentrations of aerosols were conducted in Yokohama, Japan, using the diffusion charging method. $PM_{2.5}$ mass concentration and black carbon concentration in $PM_{2.5}$ were also measured. The 24-hour continuous measurement campaigns were conducted 39 times from March to November, 2014. The surface area concentration was more closely correlated with the black carbon concentration than with the $PM_{2.5}$ mass concentration. It is considered that the abundance of black carbon particles significantly affects the surface area concentration of $PM_{2.5}$. The strength of the correlation between the surface area and black carbon concentrations varied considerably among the measurement campaigns. A relatively weaker afternoon correlation was observed compared with the other time zones (morning, evening, and night). We consider that these phenomena are due to the transportation/formation of the particles other than black carbon that affects surface area concentration and/or the variation of the surface condition of the black carbon particles.

• 천문학회보
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• 제40권1호
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• pp.86.3-86.3
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• 2015

There could be significant numbers of isolated stellar mass black holes in our Galaxy. The detection of these black holes will provide important clues on the origin of supermassive black holes. Interstellar gas will be accreted to these isolated black holes in nearly spherical flow. The gas and the interstellar magnetic field will be compressed and emit bremsstrahlung and magnetic bremsstrahlung. We calculate the density, temperature, magnetic field of the accretion flow onto a 10 solar mass black hole as well as its radiative emission; special attention is given to cyclotron radiation and synchrotron radiation, which covers from microwave to X-ray. We consider the possibility to detect these radiation from isolated Galactic black holes with current instruments and surveys.

• 천문학논총
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• 제25권3호
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• pp.77-82
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• 2010

Recent results from large surveys of the local universe show that the galaxy-black hole connection is linked to host morphology at a fundamental level and that there are two fundamentally different modes of black hole growth. The fraction of early-type galaxies with actively growing black holes, and therefore the AGN duty cycle, declines significantly with increasing black hole mass. Late-type galaxies exhibit the opposite trend: the fraction of actively growing black holes increases with black hole mass. Issues of AGN selection bias and prospects for near-future efforts with high redshift data are discussed.

• 천문학회보
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• 제38권2호
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• pp.60.1-60.1
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• 2013

We study tidal disruption and subsequent mass fallback process for stars approaching supermassive black holes on bound orbits, by performing three dimensional Smoothed Particle Hydrodynamics simulations with a pseudo-Newtonian potential. We find that the mass fallback rate decays with the expected -5/3 power of time for parabolic orbits, albeit with a slight deviation due to the self-gravity of the stellar debris. For eccentric orbits, however, there is a critical value of the orbital eccentricity, significantly below which all of the stellar debris is bound to the supermassive black hole. All the mass therefore falls back to the supermassive black hole in a much shorter time than in the standard, parabolic case. The resultant mass fallback rate considerably exceeds the Eddington accretion rate and substantially differs from the -5/3 power of time. We also show that general relativistic precession is crucial for accretion disk formation via circularization of stellar debris from stars on moderately eccentric orbits.

• 자원리싸이클링
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• 제31권6호
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• pp.81-91
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• 2022

리튬이온 배터리의 사용은 전자기기 및 전기차 등의 생산량 증가로 인해 사용량이 크게 증가하고 있으며, 이와 맞물려 향후 폐배터리의 발생량 증가도 예상된다. 따라서 폐배터리를 구성하고 있는 여러 유가 자원 중 Ni, Co, Mn, Li 등이 함유되어 있는 양극 활물질이 매우 중요한 유가 자원으로, 이를 재활용하기 위한 많은 연구가 진행되고 있다. 양극 활물질 회수를 위해서 일반적으로 폐배터리로부터 블랙 매스(Black mass)를 회수하고, 이를 처리하여 주요 금속 자원을 회수한다. 블랙 매스를 회수하는 공정은 폐배터리를 수거-방전-해체-파쇄-분급의 순서로 이루어지며, 본 연구에서는 블랙 매스 회수를 위한 파쇄/분급 공정을 분석하였다. 파쇄/분급 공정을 통해 다양한 공정 산물의 입도 특성을 분석하고, 이 과정에서 생산된 산물의 입도별 형상을 현미경 및 SEM(Scanning Electron Microscopy)-EDS(Energy Dispersive Spectrometer)로 분석하였다. 분석 결과 블랙 매스로 회수되는 입자 중 74 ㎛의 미세한 입자들은 양극/음극 활물질이 전극으로부터 단체분리되어 존재하였지만, 100 ㎛ 이상의 입자들은 전극과 활물질이 붙어있는 상태에서 파쇄에 의해 입도가 감소되어 존재함을 확인하였다. 또한 배터리의 특징인 2종 혼합물(전극과 활물질)이 결합되어 있는 시료에 대해 파분쇄 특성을 모사할 수 있는 PBM(Population Balance Model) 을 개발하였으며, 2종 혼합물의 분쇄 상수를 도출하고 입도 분포 예측 성능을 검증하였다.

• 자원리싸이클링
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• 제33권1호
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• pp.58-68
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• 2024

핵심광물인 니켈, 코발트, 리튬은 NCM계 리튬이온배터리(이하 LIB)의 양극소재로 알려져 있다. 탄소중립 기조에 따라 전기자동차의 보급량 증가로 핵심광물 수요도 증가할 것으로 예상된다. 하지만, LIB용 핵심광물 Li, Co, Ni의 수요대비 공급 부족으로 인해, 폐리튬이온배터리(EOL LIB)의 리싸이클링 수요가 증가할 것으로 예상된다. EOL LIB(폐 LIB) 재활용은 유해화학물질 무기산 침출제인 염산(HCl), 질산(HNO₃), 황산(H₂SO₄)을 침출공정에 적용하여 재활용한다. 본 연구에서는 친환경 대체침출제 메탄술폰산(이하 MSA)의 적용 가능성을 검토하였다. 또한, 침출제 농도, 환원제 농도, 침출시간, 광액농도(P/D), 온도 등의 침출인자가 NCM Black mass 침출에 미치는 영향을 연구하였다. 침출실험 결과, 침출제와 환원제 농도, 침출시간, 침출온도가 증가함에 따라 목적금속 Ni, Li, Co, Mn의 침출률이 향상됨을 확인하였고, 금속의 최대 침출률은 80℃에서 99% 이상으로 나타났다. 또한, MSA는 NCM Black mass 대상 침출에 적용하여 Ni, Li, Co, Mn을 회수할 수 있음을 확인하였다.

• 천문학회보
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• 제35권1호
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• pp.79-79
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• 2010

To investigate whether the present-day active galaxies follow the same black hole mass vs. stellar velocity dispersion (MBH-$\sigma*$) relation as quiescent galaxies, we measured the velocity dispersions of a sample of local Seyfert 1 galaxies, for which black hole masses were measured via reverberation mapping. We measured stellar velocity dispersions from high S/N optical spectra centered on the Ca II triplet region (${\sim}8500^{\circ}A$), obtained at the Keck, Palomar, and Lick Observatories. For two objects, in which the Ca II triplet region was contaminated by nuclear emission, we used high-quality H-band spectra obtained with the OH-Suppressing Infrared Imaging Spectrograph and laser-guide star adaptive optics at the Keck-II Telescope. Combining our new measurements with data from the literature, we assemble a sample of 24 active galaxies with stellar velocity dispersions and reverberation MBH in the range of black hole mass 106< MBH /$M{\odot}$ < 109,toobtainthefirstreverberationmappingconstraintsontheslopeandintrinsicscatteroftheMBH- $\sigma*$ relation of active galaxies. Assuming a constant virial coefficient f for the reverberation MBH, we find a slope ${\beta}=3.55{\pm}0.60$ and the intrinsic scatter ${\sigma}int=0.43{\pm}0.08$ dex in the relation log (MBH/M${\odot}$)=$\alpha+\beta$ log(${\sigma}*$/200 km s-1), which are consistent with those found for quiescent galaxies. We derive an updated value of the virial coefficient f by finding the value which places the reverberation masses in best agreement with the MBH - $\sigma*$ relation of quiescent galaxies; using the quiescent MBH - $\sigma*$ relation determined by Gultekin et al. we find log f=0.72+0.09 (or $0.71{\pm}0.10$) with an intrinsic scatter of $0.44{\pm}0.07$ (or 0.46+0.07) dex. No correlations between f and parameters connected to the physics of accretion (such as the Eddington ratio or line-shape measurements) are found. The uncertainty of the virial coefficient remains one of the main sources of the uncertainty in black hole mass determination using reverberation mapping, and therefore also in single-epoch spectroscopic estimates of black hole masses in active galaxies.

• 천문학논총
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• 제7권1호
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• pp.89-96
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• 1992

Recent spectroscopic observations indicate concentration of dark masses in the nuclei of nearby galaxies. This has been usually interpreted as the presence of massive black holes in these nuclei. Alternative explanations such as the dark cluster composed of low mass stars (brown dwarfs) or dark stellar remnants are possible provided that these systems can be stably maintained for the age of galaxies. For the case of low mass star cluster, mass of individual stars can grow to that of conventional stars in collision time scale. The requirement of collision time scale being shorter than the Hubble time gives the minimum cluster size. For typical conditions of M31 or M32, the half-mass radii of dark clusters can be as small as 0.1 arcsecond. For the case of clusters composed of stellar remnants, core-collapse and post-collapse expansion are required to take place in longer than Hubble time. Simple estimates reveal that the size of these clusters also can be small enough that no contradiction with observational data exists for the clusters made of white dwarfs or neutron stars. We then considered the possible outcomes of interactions between the black hole and the surrounding stellar system. Under typical conditions of M31 or M32, tidal disruption will occur every $10^3$ to $10^4$ years. We present a simple scenario for the evolution of stellar debris based on basic principles. While the accretion of stellar material could produce large amount of radiation so that the mass-to-light ratio can become too small compared to observational values it is too early to rule out the black hole model because the black hole can consume most of the stellar debris in time scale much shorter than mean time between two successive tidal disruptions. Finally we outline recent effort to simulate the process of tidal disruption and subsequent evolution of the stellar debris numerically using Smoothed Particle Hydrodynamics technique.

• 천문학회보
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• 제42권1호
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• pp.43.1-43.1
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• 2017

We investigate properties of black hole (BH) binaries formed in globular clusters, by using direct N-body simulations. Comparing with previous studies which usually considered single BH masses, our models consist of two-component BH masses, or continuous BH mass function with single mass ordinary cluster stars. During the early stage of dynamical evolution, initially distributed BHs are move to the cluster center by dynamical friction, then BH-BH binaries start to be formed, and eventually be ejected from the cluster due to three body interaction. Finally we find the formation efficiency of high mass BHs are alwats larger than that of lower mass BHs, implying that a BH mass spectrum expected from GW observation should be biased to high mass. In addition, mass ratios of BHs in binaries prefer similar masses (ratio~1), while the most extreme case is less than 3. Expected merger rate from our models is about 7 BH-BH mergers per $Mpc^3$ per yr.