• 천문학회보
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• 제46권1호
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• pp.43.1-43.1
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• 2021

In this study, we suggest a new method to estimate the mass of a halo coronal mass ejection (CME) using synthetic CMEs. For this, we generate synthetic CMEs based on two assumptions: (1) the CME structure is a full ice-cream cone, (2) the CME electron density follows a power-law distribution (ρ_cme=ρ₀r^-n). The power-law exponent n is obtained by minimizing the root mean square error between the electron number density distributions of an observed CME and the corresponding synthetic CME at a position angle of the CME leading edge. By applying this methodology to 57 halo CMEs, we estimate two kinds of synthetic CME mass. One is a synthetic CME mass which considers only the observed CME region (M_cme1), the other is a synthetic CME mass which includes both the observed CME region and the occulted area larger than 4 solar radii (M_cme2). From these two cases, we derive conversion factors which are the ratio of a synthetic CME mass to an observed CME mass. The conversion factor for M_cme1 ranges from 1.4 to 3.0 and its average is 2.0. For M_cme2, the factor ranges from 1.8 to 5.0 with the average of 3.0. These results imply that the observed halo CME mass can be underestimated by about 2 times when we consider the observed CME region, and about 3 times when we consider the region including the occulted area. Interestingly these conversion factors have a very strong negative correlation with angular widths of halo CMEs.We also compare the results with the CME mass estimated from STEREO observations.

• 전자공학회논문지
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• 제52권4호
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• pp.3-8
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• 2015

이 논문에서는 신호점 매칭 오차(constellation-matched error: CME)와 비 신호점 매칭 오차(non-constellation-matched error: non-CME)를 선형 결합한 오차 신호 기반의 블라인드 등화 알고리즘을 제안한다. 새로운 오차 신호는 초기 수렴을 달성하기 위한 non-CME 항과 출력 신호의 심볼간 간섭(intersymbol interference: ISI) 성능을 개선하기 위한 CME 항을 포함하도록 설계되었고, 결합 인자를 통해 두 오차 항을 제어한다. 오차 항을 제어하여 등화 단계에 적합한 오차 신호를 발생함으로써 기존 알고리즘에 비해 수렴 속도와 심볼간 간섭 제거 성능을 개선하였다. 다중경로 채널에 잡음을 부가한 조건하에서 이루어진 64-QAM과 256-QAM 신호에 대한 모의실험에서 제안 방법이 CMA와 CMA+DD 동시 등화에 비해 우수한 것으로 나타났다.

• 천문학회보
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• 제36권1호
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• pp.39.2-39.2
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• 2011

In this study we have examined the occurrence probability of solar proton events (SEPs) and their peak fluxes depending two CME parameters, linear speed and angular width. For this we used the NOAA SPE events and their associated CME data from 1997 to 2006. As a result, the probability strongly depends on two parameters as follows. In the case of halo CME whose speed is equal to and faster than 1500km/s, 36.1% are associated with SPEs but in the case of partial halo CME ($120^{\circ}{\leq}AW$ < $359^{\circ}$) whose speed is $400{\leq}V$ < $1000km/s$, only 0.9% are associated with SPEs. When we consider only front-side CMEs, 45.3% are associated with SPEs in the first case and 1.8% are associated with them in the second case. Both of whole CME data group and front-side CME data group have similar tendencies. The probabilities are different as much as 4.9 to 23 times according to the CME speed and 1.6 to 6.5 times to the angular width. We have also examined the relationship between CME speed and proton peak flux as well as its dependence on angular width (partial halo CME and halo CME), longitude (east, center, and west) and direction parameter (< 0.4 and {\geq} 0.4). Our results show that the relationships strongly depend on longitude as well as direction parameter. In addition, the relationship using the radial CME speed based on a cone model has a higher correlation coefficient than that using the projected CME speed.

• 천문학회보
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• 제44권2호
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• pp.43.3-43.3
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• 2019

A coronal mass ejection (CME) mass is generally estimated by the total brightness measured from white-light coronagraph observations. The total brightness are determined from the integration of the Thomson scattering by free electrons of solar corona along the line of sight. It is difficult to estimate the masses of halo CMEs due to the projection effect. To solve this issue, we construct a synthetic halo CME with a power-law density distribution (ρ = ρ₀r^-3) based on a full ice-cream cone model using SOHO/LASCO C3 observations. Then we compute a conversion factor from observed CME mass to CME mass for each CME. The final CME mass is determined as their average value of several CME masses above 10 solar radii. Our preliminary analysis for six CMEs show that their CME mass are well determined within the mean absolute relative error in the range of 4 to 15 %.

• 한국정보전자통신기술학회논문지
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• 제2권3호
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• pp.87-95
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• 2009

정보이론적 학습 기법에 해당하는 에러 엔트로피 최소화 (MEE) 성능기준과 상호 상관 엔트로피 최대화 (MCC) 성능기준은 그 동안 깊이 있게 많은 연구가 이루어져 왔다. 에러 엔트로피 최소화 성능기준은 정보 포텐셜을 최대화하는 것으로 귀결되고 상호 상관 엔트로피 최대화 성능기준은 시스템의 출력과 원신호의 상호 상관도를 최대화하는 것으로 정의된다. 이 두 성능기준을적정 가중치를 두고 합성한 것이 기준점을 내포한 에러 엔트로피 최소화 기법 (MEEF) 인데 이 또한 많은 연구가 이루어지고 있다. 이 논문에서는 블라인드 채널 등화를 위해 CMA에 쓰이는 상수 모듈러스 에러 (CME)를 도입하여 이 정보이론적 학습기법에 적용하고자 그 가능성과 문제점을 찾고자 연구하였다. 또한 MEEF 성능기준에도 이 CME 적용가능성을 연구하였다. 연구결과로부터 CME를 적용한 MEE (MEE-CME)는 상수 모듈러스 정보를 잃게 되는 결과를 낳았다. 이 결과 MEE-CME나 MEE를 사용하는 MEEF-CME 모두에게서 수렴하지 못하거나 CME를 사용하는 다른 방식과 비교할 때 수렴이 늦게 되는 문제점을 발견하게 되었다.

• Journal of Microbiology and Biotechnology
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• 제31권12호
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• pp.1656-1666
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• 2021

Dental pathogens lead to chronic diseases like periodontitis, which causes loss of teeth. Here, we examined the plausible antibacterial efficacy of copper nanoparticles (CuNPs) synthesized using Cupressus macrocarpa extract (CME) against periodontitis-causing bacteria. The antimicrobial properties of CME-CuNPs were then assessed against oral microbes (M. luteus. B. subtilis, P. aerioginosa) that cause periodontal disease and were identified using morphological/ biochemical analysis, and 16S-rRNA techniques. The CME-CuNPs were characterized, and accordingly, the peak found at 577 nm using UV-Vis spectrometer showed the formation of stable CME-CuNPs. Also, the results revealed the formation of spherical and oblong monodispersed CME-CuNPs with sizes ranged from 11.3 to 22.4 nm. The FTIR analysis suggested that the CME contains reducing agents that consequently had a role in Cu reduction and CME-CuNP formation. Furthermore, the CME-CuNPs exhibited potent antimicrobial efficacy against different isolates which was superior to the reported values in literature. The antibacterial efficacy of CME-CuNPs on oral bacteria was compared to the synergistic solution of clindamycin with CME-CuNPs. The solution exhibited a superior capacity to prevent bacterial growth. Minimum inhibitory concentration (MIC), minimum bactericidal concentration (MBC), and fractional inhibitory concentration (FIC) of CME-CuNPs with clindamycin recorded against the selected periodontal disease-causing microorganisms were observed between the range of 2.6-3.6 ㎍/ml, 4-5 ㎍/ml and 0.312-0.5, respectively. Finally, the synergistic antimicrobial efficacy exhibited by CME-CuNPs with clindamycin against the tested strains could be useful for the future development of more effective treatments to control dental diseases.

• Journal of Astronomy and Space Sciences
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• 제15권2호
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• pp.307-320
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• 1998

다중 위성 관측을 이용하여 지구 근처에서의 태양물질 방출현상(CME: Coronal Mass Ejection)의 전파 속도와 방향에 대하여 조사하였다. 이를 위해 1994년 11월까지 지구에 영향을 미친 CME 중에서 세 개 이상의 위성에서 관측되고 각 위성들이 충분한 거리를 두고 떨어져 있는 1997년 1월 6-11일과 1997년 11월 4-7일의 두 CME 자료를 선택하였다. 위성들의 위치를 공통 좌표 계로 전환하여 위성간의 거리와 CME에 의한 물리량의 변화 시간을 조사하여 CME의 전파 방향과 속도를 계산하였다. 선택된 자료에 대한 조사 결과 지구 자기권 내부에서 CME 전파 속도가 급격히 줄어들었으며 또한 자기권 외부에서의 CME 전파 방향이 GSE 좌표계상의 -x 방향과 일치함을 알 수 있었다.

• 천문학회보
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• 제37권1호
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• pp.97-97
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• 2012

Hinode/XRT has observed coronal mass ejections (CMEs) since it launched on Sep. 2006. Observing programs of Hinode/XRT, called 'CME watch', perform several binned observations to obtain large FOV observations with long exposure time that allows the detection of faint CME plasmas in high temperatures. Using those observations, we determine the upper limit to the mass of hot CME plasma using emission measure by assuming the observed plasma structure. In some events, an associated prominence eruption and CME plasma were observed in EUV observations as absorption or emission features. The absorption feature provides the lower limit to the cold mass while the emission feature provides the upper limit to the mass of observed CME plasma in X-ray and EUV passbands. In addition, some events were observed by coronagraph observations (SOHO/LASCO, STEREO/COR1) that allow the determination of total CME mass. However, some events were not observed by the coronagraphs possibly because of low density of the CME plasma. We present the mass constraints of CME plasma and associated prominence as determined by emission and absorption in EUV and X-ray passbands, then compare this mass to the total CME mass as derived from coronagraphs.

• 천문학회보
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• 제42권2호
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• pp.62.1-62.1
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• 2017

In space weather forecast, it is important to determine three-dimensional properties of CMEs. Using 29 limb CMEs, we examine which cone type is close to a CME three-dimensional structure. We find that most CMEs have near full ice-cream cone structure which is a symmetrical circular cone combined with a hemisphere. We develop a full ice-cream cone model based on a new methodology that the full ice-cream cone consists of many flat cones with different heights and angular widths. By applying this model to 12 SOHO/LASCO halo CMEs, we find that 3D parameters from our method are similar to those from other stereoscopic methods (i.e., a triangulation method and a Graduated Cylindrical Shell model). In addition, we derive CME mean density (${\bar{\rho}_{CME}}={\frac{M_{total}}{V_{cone}}}$) based on the full ice-cream cone structure. For several limb events, we determine CME mass by applying the Solarsoft procedure (e.g., cme_mass.pro) to SOHO/LASCO C3 images. CME volumes are estimated from the full ice-cream cone structure. For the first time, we derive average CME densities as a function of CME height for several CMEs, which are well fitted to power-law functions. We will compare densities (front and average) of geoeffective CMEs and their corresponding ICME ones.

• 천문학회보
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• 제44권1호
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• pp.50.1-50.1
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• 2019

In coronagraph images, it is often observed that two successive CMEs merge into one another and form complex structures. This phenomenon, so called CME cannibalism caused by the differences in ejecting times and propagating velocities, can significantly degrade forecast capability of space weather, especially if it occur near the Earth. Regarding this, we attempt to analyze the cases that two CMEs are expecting to meet around 1 AU based on their arrival times. For this, we select 13 CME-CME pairs detected by ACE, Wind and/or STEREO-A/B. We find that 8 CME-CME pairs show a shock structure, which means they already met and became one structure. Meanwhile 5 pairs clearly show magnetic holes between two respective shock structures. Based on detailed investigation for each pair and statistical analysis for all events, we can get clues for following questions: 1) How does the solar wind structure change when they are merging? 2) Are there any systematic characteristics of merging process according to the CME properties? 3) Is the merging process associated with the occurrence of energetic storm particles? 4) What causes errors in calculating CME arrival times? Our results and discussions can be helpful to understand energetic phenomena not only close to the Sun but also near the Earth.