• 천문학회보
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• 제25권2호
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• pp.50-50
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• 2000

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 1999년도 한국우주과학회보 제8권2호
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• pp.80-80
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• 1999

No Abstract, See Full Text

• 천문학회보
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• 제30권1호
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• pp.35.2-35.2
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• 2005

• 한국건설순환자원학회논문집
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• 제9권4호
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• pp.405-412
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• 2021

본 연구는 건설폐기물 중간처리 사업장에서 발생하는 미세먼지의 환경영향을 조사하여, 향후 예상되는 정부의 강화된 환경규제에 공학적 자료 및 미세먼지 발생 억제 방안 제시를 목적으로 한다. 연구 결론은 다음과 같다. 1) 사업장 내의 미세먼지 농도측정 결과, 파분쇄 작업이 이루어지는 지점에서 최대치인 160㎍/m³가 측정되었으며, 폐기물 하적되는 지점이 두 번째로 높게 나타나, 향후 집중적인 발생 억제 방안의 적용이 필요하다. 2) 사업장 내 젖은 도로 상태는 113㎍/m³, 건조된 상태 때는 50㎍/m³의 미세먼지 농도가 측정되어, 살수만으로도 미세먼지를 50% 정도는 감소시키는 것으로 나타났다. 3) 이격에 따른 영향을 분석한 결과, 작업장 가동 중의 PM10은 사업장에서 인근 지역과 비교하여 약 25㎍/m³ 높게 측정되었으며, PM2.5의 경우는 인근 지역과 뚜렷한 차이가 없는 것으로 나타났다. 4) 중금속 함유량을 측정한 결과는 인근 지역에 영향을 주지 않는 것으로 나타났다.

• 천문학회보
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• 제37권2호
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• pp.98.2-98.2
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• 2012

We firstly present the unified Far-UV continuum map of the Taurus-Auriga-Perseus (TPA) complex, one of the largest local associations of dark cloud located in (l, b)=([154,180], [-28, -2]), by merging both FIMS and GALEX. The FUV continuum map shows that dust extinction correlate well with the FUV around the complex. It shows strong absorption in FUV toward the dense Taurus cloud while it does not in California cloud. It turned out that it is related to the relative location of each cloud and Perseus OB2 association. We also present some results of dust scattering simulation based on Monte Carlo Radiative Transfer technique (MCRT). Through this dust scattering simulation, we have derived the scattering parameter for this region, albedo(a)=$0.42^{+0.05}{_{-0.05}}$, asymmetry factor(g)=$0.47^{+0.11}{_{-0.27}}$. The optical parameters we obtained seem reasonable compared to the theoretical model values ~0.40 and ~0.65 for the albedo and the phase function though the phase function is rather small. Using the result of simulation, we figured out the geometries of each cloud in the complex region, especially their distances and thicknesses. Our predictions from the results are in good agreement with the previous studies related to the TPA complex. For example, the Taurus cloud is within ~200pc from the Sun and the Perseus seems to be multi-layered, at least two. The California cloud is more distant than the other cloud on average at ~350 pc and Auriga cloud seems to be between the Taurus cloud and the eastern end of the California cloud. We figured out that across the TPA complex region, there might be some correlation between the LSR velocity and the distance to each cloud in the complex.

• 한국응용과학기술학회지
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• 제35권1호
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• pp.284-291
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• 2018

본 연구에서는 식품 및 화장품 원료로 널리 사용되는 천연 다당류의 분자 구조, 분자량, 점도, 친수성, 팽창, 습윤 및 보습 특성을 이용하여 도로 분진 방지제를 제조하였다. 다양한 분진 제어 효과가 확인되었으며 단순한 물 분사 및 시험 대조군인 합성PVA보다 우수한 결과를 얻었다. 또한 수분증발 비교, 비산 저감율, 공사현장 테스트 및 물벼룩 급성 독성 시험 등의 영향을 연구하고 토양 및 수질의 안전성을 연구하여 도로 분진 방지제의 유용성을 확인하였다.

• 한국정보통신학회논문지
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• 제12권5호
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• pp.821-827
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• 2008

본 논문은 $1{\sim}20Ghz$의 대역별 위성통신 신호에 미치는 영향에 대해 예측 모델을 제안하고 기존 황사시 측정한 데이터와 비교 분석하였다. 황사의 감쇠 특성을 분석하기 위해 황사 물질에 대한 이론적 분석을 하였으며 이를 통해 예측 감쇠량을 제시하였다. 예측 감쇠량을 실제 우리나라 황사 강도와 가시거리와 높이 등의 파라미터를 적용한 이론치를 구하여 4년간 측정한 실측치와 비교하였고 이를 토대로 황사로 인한 감쇠를 미리 예측 가능할 것으로 확인되었다.

• 천문학회보
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• 제45권1호
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• pp.57.2-57.2
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• 2020

We observed the Class I protostar TMC-1A in polarized dust emission at 1.3 mm at a spatial resolution of ~40 au using ALMA. Previous observations revealed a disk (r~100 au), surrounded by an infalling envelope, and a CO outflow going in the north-south direction in TMC-1A. Our observations detected polarized dust emission in a central region (r~50 au) and ~100 au north and south of the central protostar. The former polarization is likely due to self-scattering because of the polarization direction along the disk minor axis, the polarization fraction independent of Stokes I, and a high optical thickness. The latter polarization is roughly in the outflow region. The position and direction, particularly in the north, imply multiple possible mechanisms: magnetically or mechanically aligned dust grains in the outflow or in an accretion flow.

• 한국농촌건축학회논문집
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• 제25권4호
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• pp.9-16
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• 2023

In this study, the status and characteristics of fine dust and its impact on neighboring areas were investigated to proactively respond to the government's environmental regulations expected in the future and to minimize the damage by the fine dust generated at construction waste intermediate treatment plants. In addition, since there are no such plants that can affect the surroundings with no houses or other waste treatment sites nearby, an independently located construction waste intermediate treatment plant was selected to compare the characteristics of fine dust with that from the construction waste intermediate treatment sites located in the downtown area. The conclusions of the study are as follows. (1) The measurement results of PM10 at 4 points in the plant showed that the location where the crushing facility was operating had an elevated level of fine dust at 80㎍/m³ on average and a maximum of 124㎍/m³, and the level rose to 110㎍/m³ at points where vehicles frequent. (2) The PM2.5 measurement results inside the plant showed that the average concentration of the reference point was 16㎍/m³ and the maximum value was 20㎍/m³, which was distributed within the management standard. (3) It was found that the average concentration of PM10 in the nearby area ranged from 28 to 38㎍/m³, which was similar to or lower than 36㎍/m³ of the reference point. Therefore, the concentration of the fine dust generated in the plant had a negligible effect on the increase in concentration of fine dust in nearby areas. (4) The heavy metal contents were measured from the filter paper collected from the plant. The PM10 was found to be about 14 to 26ng/m³, and PM 2.5 was 25 to 28ng/m³, which was the average of domestic atmospheric concentrations. (5) The SEM-EDX analysis results showed that the PM10 contained Si and O around 40% similarly for both. The SiO2, a component of silica occupied the most and C was present as CaCO3, which was assumed to be a limestone component. The remaining components included NaO, Al2O3, and CaO as trace oxides. (6) The SEM-EDX analysis results showed that the PM 2.5 contained 5 to 7% of Cl, which is a chlorine ion, and a small amount of K was detected at 2.51% in the sample from the shutdown plant.

• 천문학회보
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• 제37권1호
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• pp.73.1-73.1
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• 2012

We present the results of dust scattering simulations carried out for the Orion Eridanus Superbubble region by comparing them with observations made in the far-ultraviolet. The albedo and the phase function asymmetry factor (g-factor) of interstellar grains were estimated as well as the distance and thickness of the dust layers. The results are: 0.39-0.45 for the albedo and 0.25-0.65 for the g-factor, in good agreement with previous determinations and theoretical predictions. The distance of the assumed single dust layer, modeled for the Orion Molecular Cloud Complex, was estimated to be -110 pc and the thickness ranged from -130 at the core to -50 pc at the boundary for the region of the present interest, implying that the dust cloud is located in front of the Superbubble. The simulation result also indicates that a thin (-10 pc) dust shell surrounds the inner X-ray cavities of hot gas at a distance of -70-90 pc.