• 천문학논총
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• 제27권4호
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• pp.325-329
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• 2012

We will report our recent study on the properties of more than 1,600 galaxies detected by the AKARI All-Sky Survey with physical quantities based on optical and 21-cm observations, to understand the physics determining the infrared spectral energy distribution (Totani et al., 2011). We discover a tight linear correlation for normal star-forming galaxies between the radiation field strength of dust heating (corresponding to dust temperature) and the galactic-scale infrared radiation field, $L_{TIR}/R^2$. This is the tightest correlation of dust temperature ever known, and the dispersion along the mean relation is 13% in dust temperature. This relation can be explained physically by a thin layer of heating sources embedded in a thicker, optically-thick dust screen. We also find that the number of galaxies sharply drops when galaxies become optically thin against dust-heating radiation, indicating that a feedback process to galaxy formation (e.g., by the photoelectric heating) is working when dust-heating radiation is not self-shielded on a galactic scale. We discuss implications from these findings for the $M_{H_I}$ -size relation, the Kennicutt-Schmidt relation, and galaxy formation in the cosmological context.

• 천문학회보
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• 제37권1호
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• pp.74.1-74.1
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• 2012

It is known that the diffuse H${\alpha}$ halos around bright H II regions are more extended than the dust-scattered halos around point sources and the line ratios [S II] ${\lambda}$6716/H${\alpha}$ and [N II] ${\lambda}$6583/H${\alpha}$ observed outside of bright H II regions are generally higher than those in H II regions. These observational facts have been regarded as evidence against the dust-scattering origin of the diffuse H${\alpha}$ emission and the effect of dust-scattering has been neglected in studying the diffuse H${\alpha}$ emission. In this paper, we find, however, that dust-scattered halos of H II regions should be more extended than those of point sources and is in good agreement with the observed H${\alpha}$ profiles around H II regions. We also found that the observed line ratios [S II]/H${\alpha}$, [N II]/H${\alpha}$, and He I ${\lambda}$5876/H${\alpha}$ in the diffuse regions can be well reproduced with the dust-scattered halos around H II regions which are photoionized by late O- and/or early B-type stars in the interstellar medium with the abundances close to those of the warm neutral medium. Therefore, we conclude that the diffuse H${\alpha}$ emission may originate mostly from the dust-scattering.

• 천문학회보
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• 제35권2호
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• pp.35.2-35.2
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• 2010

It is crucial to understand the dust properties in the early universe since they provide important clues about how the early cosmic star formation should be interpreted in the presence of dust extinction. GRB 071025 is an unusually red GRB that occured at high redshift, offering an unique opportunity to study the dust properties in the early universe. We investigate the extinction properties of GRB 071025 through the analysis of RIJHK data obtained with the 1-m telescope at Mt. Lemmon Optical Astronomy Observatory (LOAO) and Simultaneous Quad Infrared Imaging Device (SQIID) on the Kitt-Peak Mayall 4-m telescope. Our dataset is independent from that in a previous work (Perley et al. 2010) where a small systematic photometric errors could complicate the interpretation. After determining the temporal power law exponent with five I-band frames from LOAO, we construct a multi-band monochromatic SED of the GRB afterglow. By using various extinction laws, we find that the SED is best fitted with models that incorporate SNe II dust and derive a photometric redshift of 4.99(+0.12/-0.03). Our results strongly support the prior claim that dusts in GRB 071025 originate mainly from supernovae, implying SNe II predominantly contributed to the dust enrichment in the early universe (z ~ 5).

• Journal of Astronomy and Space Sciences
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• 제23권1호
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• pp.11-18
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• 2006

비정질규산염과 비정질탄소 먼지입자들이 혼합된 불투명계수를 사용하여. 규산염탄소항성의 구형대칭 먼지층에 대한 복사전달 모형계산을 진행하였다. 계산결과들을 적외선 관측자료와 자세히 비교하여 최적의 모형 계수들을 얻어내었고 규산염탄소항성과 그 먼지층의 물리적,화학적 구조에 대한 해석에 적용하였다. 이 연구에 사용된 4개의 항성들은 먼지충의 화학성분이 변하는 과도기의 특징들을 다양하게 나타내었다. 단순히 규산염으로 이루어져 있지만 항성 표면으로부터 많이 떨어져 있는 먼지층은 홑별로서의 과도기 규산염탄소항성의 전형적인 모습이다. 그러나 쌍성일 경우 전시대의 규산염과 이후의 탄소 먼지입자들이 공존하는 독특한 특징을 보일 수 있다.

• 천문학회보
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• 제37권2호
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• pp.140.2-140.2
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• 2012

The silicate carbon star IRAS 09425-6040 shows very conspicuous crystalline silicate dust features and excessive emission at far infrared. To investigate properties of dusty envelopes around the object, we use radiative transfer models for axisymmetric and sphericallly symmetric dust distributions. We perform model calculations for various possible combinations of dust shells and disks with various dust species. We compare the model results with the observed spectral energy distributions (SEDs) including the IRAS, ISO, AKARI, MSX and 2MASS data. We find that a model with multiple disks of amorphous and crystalline silicate and multiple spherical shells of carbon dust can reproduce the observed SED fairly well. This supports the scenario for the origin of silicate carbon stars that oxygen-rich material was shed by mass loss when the primary star was an M giant and the O-rich material is stored in a circumbinary disk. Highly (about 75 %) crystallized forsterite dust in the disk can reproduce the conspicuous crystalline features of the ISO observational data. This object looks to have a detached silicate and H2O ice shell with a much higher mass-loss rate. It could be a remnant of the chemical transition phase. The last phase of stellar winds of O-rich materials looks to be a superwind.

• 항공우주기술
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• 제12권2호
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• pp.99-107
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• 2013

화성은 국지적인 강한 바람과 그 바람에 의해 표면의 먼지들이 솟아오르는 현상들을 가지고 있다. 대기 순환과 먼지 상승은 서로 관계가 있다고는 알려져 있지만, 먼지 상승의 역학적 원인은 명확하게 밝혀진 것은 없다. 먼지 폭풍은 히말라야 산 높이까지 상승하는 매우 강한 상승 기류인데 이런 기류들은 탐사선이 착륙할 때 또는 로버가 탐사를 수행할 때 피해야 할 위험 요소이다. 본 연구에서는 대기 순환과 관련된 먼저 폭풍의 발생 시기와 발생 지역 분포에 대해 조사하였다. 대기 순환의 원천적인 에너지는 태양이기 때문에 먼지 폭풍의 발생 시기와 화성의 계절에 대해 분석하였고, 최종적으로는 발생 시기와 발생 지역의 공간 분포의 관계를 지도로 작성하였다. 이 자료를 토대로 화성 먼지 폭풍의 발생이 빈번하지 않은 지역과 시기를 예측할 수 있다. 향후 이 자료는 국내 자력으로 화성 착륙선을 보낼 때 착륙시기와 관계하여 발사시점 및 착륙지점을 선정하는데 있어서 결정적인 역할을 할 것이라고 기대한다.

• 한국안전학회지
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• 제31권4호
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• pp.55-63
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• 2016

A dust explosion is a phenomenon of strong blast wave propagation involving destruction which results from dust pyrolysis and rapid oxidation in a confined space. There has been some research done to find individual explosion characteristics and common physical laws for various dust types. However, there has been insufficient number of studies related to the heat of combustion of materials and the oxygen consumption energy about materials in respect of dust explosion characteristics. The present study focuses on the relationship between dust explosion characteristics of wood dust samples and oxygen consumption energy. Since it is difficult to estimate the weight of suspended dust participating in explosions in dust explosion and mixtures are in fuel-rich conditions concentrations with equivalent ratios exceeding 1, methods for estimating explosion overpressure by applying oxygen consumption energy based on unit volume air at standard atmospheric pressure and temperature are proposed. In this study an oxygen consumption energy model for dust explosion is developed, and by applying this model to TNT equivalent model, initial explosion efficiency was calculated by comparing the results of standardized dust explosion experiments.

• 대한전자공학회:학술대회논문집
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• 대한전자공학회 2001년도 The 6th International Symposium of East Asian Resources Recycling Technology
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• pp.365-369
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• 2001

EAF's dust has been treated mainly by pyrometallurgical reduction process in rotary kiln furnace to recover valuable metal elements such as Zn and to avoid the disposal of hazardous materials to waste. Recently, hydrometallurgical eletrowinning of zinc from a zinc-amino chloride solution obtained by the leaching of EAF's dust was developed to recover high grade zinc metal from EAF’s dust. But there are some disadvantages in each process such as difficulty of operation condition control and sticking problem in kiln process and low extractability and recovery of zinc owing to insoluble zinc-ferrite in electrowinning process. We propose a new combined process of pyrometallurgical one and hydrometallurgical one to treat EAF's dust efficiently and economically. In this study, ammonium chloride solution leaching of crude zinc oxide recovered from reduction of EAF's dust was carried out to find out the efficiency of zinc extraction from it and the possibility for performance of eletrowinning in the proposed process. Effects of various leaching variables ruck as leaching temperature, concentration of leaching solution and leaching time were investigated. And the leaching results of the crude zinc oxide were compared with those of EAF's dust. The extraction percents of zinc in ammonium chloride solution leaching of the crude zinc oxide recovered from reduction of EAF's dust were above 80% after 60 minutes of leaching under the leaching condition of 4M NH$_4$CI concentration and above leaching temperature of 7$0^{\circ}C$. And the concentrations of zinc in the leached solution were obtained above 50g/$\ell$. The activation energy calculated for zinc extraction in NH$_4$CI leaching was 58.1 KJ/㏖ for EAF's dust and 15.8 KJ/㏖ for the crude zinc oxide recovered from reduction of EAF's dust.

• 한국화재소방학회논문지
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• 제13권4호
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• pp.7-12
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• 1999

석유 화학플랜트에서 다량 부산되는 가연성 고체인 EVA(ethyl vinyl acetate) 분진의 열적특성 및 산화제와의 혼촉 위험성을 조사하였다. 시차주사열량계(DSC, Differential Scanning calorimeter) 및 열중량 분석기(TGA, Thermogavimetric Analysis)를 이용하여 온도에 따른 발열개시온도 및 중량감소를 조사하였고, EVA 분진의 위험성을 살펴보고자 몇 가지 대표적인 산화제와 혼합하여 무게비에 따른 압력용기 내에서의 혼촉 위험성을 조사하였다. DSC 분석 결과 EVA 분진의 열분해에 따른 발열 peak가 220~$250^{\circ}$ 부근에서 나타나고 있으며, TGA 분석결과 EVA 분진의 분해온도는 250~$500^{\circ}$ 범위이다. 압력 용기 시험에 의한 산화제와 EVA 분진의 혼촉 위험성은 오리피스 직경이 감소할수록 증가하며, 승온속도가 증가할수록 증가한다. 또한 승온속도가 느린 경우에는 시료의 분해온도와 산화제의 분해온도가 비슷한 경우 혼촉 위험성이 크게 나타났으며, 승온속도가 빠른 경우에는 시료 및 산화제의 분해온도보다는 분자 내에 산소의 함유량이 높은 산화제가 혼촉 위험성이 크게 나타났다.

• 천문학회보
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• 제36권1호
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• pp.88.2-88.2
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• 2011

The far-ultraviolet (FUV) continuum and spectral images of C IV and H2 emission lines for the region of Orion-Eridanus Superbubble (OES) are hereby presented and compared with the maps obtained in other wavelengths. While the region shows complex structures, consisting of hot gases and cold dust, a close examination reveals that the FUV emission in this region can be understood reasonably as the result of their interactions. We confirm the origin of most diffuse FUV continuum to be starlight scattered by dust, but we also find that the ionized gas also contributes 50-70% of the total FUV intensity in the regions of H_alpha arcs. We note the bright diffuse FUV continuum in the eastern part of the northern dust-rich region, and attribute it to the bright early-type stars more abundant in this region than in the west as the amount of dust itself does not seem to be much different across 'arc A' that separates the two regions. In addition, two P Cygni-type stars are identified in this eastern region and their peculiar spectral profiles around the C IV emission line are anifested in the scattered diffuse spectrum. Besides this, the C IV emission is generally enhanced at the boundaries of the hot X-ray cavities where thin dust regions are located, confirming the thermal interface nature of the origin of this cooling emission line. The morphology of the H2 emission shows a general correlation with dust extinction features but its intensity peaks are rather located in thin dust areas, off the peak dust regions. Furthermore, H2 emission is seen to be weak in the arc A region though the arc passes through the center of the dust-rich area. Hence, the H2 emission and dust features, together with those of X-ray and ion lines emissions, show stratified structure of arc A quite well, again confirming its thermal interface nature.