• Journal of Astronomy and Space Sciences
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• 제27권4호
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• pp.329-335
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• 2010

We investigate the sources of the variation of the high-latitude thermospheric neutral mass density depending on the interplanetary magnetic field (IMF) conditions. For this purpose, we have carried out the National Center for Atmospheric Research Thermosphere-Ionosphere Electrodynamics General Circulation Model (NCAR-TIEGCM) simulations for various IMF conditions under summer condition in the southern hemisphere. The NCAR-TIEGCM is combined with a new empirical model that provides a forcing to the thermosphere in high latitudes. The difference of the high-latitude thermospheric neutral mass density (subtraction of the values for zero IMF condition from the values for non-zero IMF conditions) shows a dependence on the IMF condition: For negative $B_y$ condition, there are significantly enhanced difference densities in the dusk sector and around midnight. Under the positive-$B_y$ condition, there is a decrease in the early morning hours including the dawn side poleward of $-70^{\circ}$. For negative $B_z$, the difference of the thermospheric densities shows a strong enhancement in the cusp region and around midnight, but decreases in the dawn sector. In the dusk sector, those values are relatively larger than those in the dawn sector. The density difference under positive-$B_z$ condition shows decreases generally. The density difference is more significant under negative-$B_z$ condition than under positive-$B_z$ condition. The dependence of the density difference on the IMF conditions in high latitudes, especially, in the dawn and dusk sectors can be explained by the effect of thermospheric winds that are associated with the ionospheric convection and vary following the direction of the IMF. In auroral and cusp regions, heating of thermosphere by ionospheric currents and/or auroral particle precipitation can be also the source of the dependence of the density difference on the IMF conditions.

• Journal of Astronomy and Space Sciences
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• 제12권2호
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• pp.168-178
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• 1995

We have modeled the dust envelopes around carbon stars with close attention to the evolution of the structure of the dust shells. We use various dust density distributions to take account the effect of the superwind due to the helium shell flash by adding a density increased region. Depending on the position and quality of the density increased region, the model results are different from the results with conventional density distribution. The new results fit the observations of some carbon stars better. The IR two-color diagrams comparing the results of the super wind models and IRAS observation of 252 carbon stars have been made. The new results can explain much wider regions on the IR two-color diagrams.

• 천문학회보
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• 제40권1호
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• pp.63.1-63.1
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• 2015

In this study, we determine coronal electron density distributions by analyzing DH type II radio observations based on the assumption: a DH type II radio burst is generated by the shock formed at a CME leading edge. For this, we consider 11 Wind/WAVES DH type II radio bursts (from 2000 to 2003 and from 2010 to 2012) associated with SOHO/LASCO limb CMEs using the following criteria: (1) the fundamental and second harmonic emission lanes are well identified; (2) its associated CME is clearly identified in the LASCO-C2 or C3 field of view at the time of type II observation. For these events, we determine the lowest frequencies of their fundamental emission lanes and the heights of their leading edges. Coronal electron density distributions are obtained by minimizing the root mean square error between the observed heights of CME leading edges and the heights of DH type II radio bursts from assumed electron density distributions. We find that the estimated coronal electron density distribution ranges from 2.5 to 10.2-fold Saito's coronal electron density models.

• 한국실내디자인학회논문집
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• 제21권5호
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• pp.343-354
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• 2012

Museums in Korea have experienced continuing quantitative growth since the late Choson Dynasty. However, a careful examination of visitors' viewing behavior has not been properly performed. Accordingly, social education for visitors in museums is not properly conducted despite the vast amount of information that museums possess. Given these circumstances, this study which focuses on the factors that influence visitors' behavior in museums intends to examine the effects that the configuration of exhibition space and the resulting visitor circulation patterns have on visitors' behavior with regard to visitor density. From this perspective, and considering five public historical museums within the seoul metropolitan area of korea, a correlation analysis has been conducted based upon quantitative analysis related to the configuration of exhibition space and visitors' observed viewing behaviors. The result of our study is that the configuration of exhibition space influences the patterns of visitor circulation, distribution of space, and the subsequent state of visitor density. Accordingly, the effects of visitor density on the viewing speed and other viewing behaviors could be identified. Based on these findings, the configurational differences in exhibition spaces were identified as one of the key factors that influence visitors' viewing behaviors.

• 한국조경학회지
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• 제25권3호
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• pp.234-245
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• 1997

This study aims to clarify the preference of the hedge, on focusing the height, density, width of the hedge, which gives limited dwelling space continuity with outer space, promotes the naturality to dwelling environment, and plays an important role as green space in city. For this, it is performed statistical analysis by field survey, by classifying the hedge as planting pattern, and synthesizing the photograph. Therefore, the results of this study are as follows : 1. In the preference of height of the hedge, when only the hedge is composed, 1.5M is preferred, and when the hedge with deciduous tree, with needle-leaf tree, 1.25M is preferred. 2. In the preference of density of the hedge, which are perfect density, in case of the hedge, which are almost density, in case of the needle-leaf tree, are preferred. 3. In the preference of width of the hedge, 0.4M is preferred. 4. In the preferential factors of the hedges, the preference of the hedge is mainly influenced by density. As the result of multiple regression analysis of visual preference as the height, the density, the width, and the regression equation are as follows : Visual Preference = 0.094+0.412(density)+0.370(height)+0.177(width)

• 천문학회보
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• 제44권1호
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• pp.50.2-50.2
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• 2019

Understanding three-dimensional structure and parameters (e.g., radial velocity, angular width, source location and density) of coronal mass ejections (CMEs) is essential for space weather forecast. In this study, we determine CME mean density in solar corona and near the Earth. We select 38 halo CMEs, which have the corresponding interplanetary CMEs (ICMEs), by SOHO/LASCO from 2000 to 2014. To estimate a CME volume, we assume that a CME structure is a full ice-cream cone which is a symmetrical circular cone combined with a hemisphere. We derive CME mean density as a function of radial height, which are approximately fitted to power-law functions. The average of power-law indexes is about 2.1 in the LASCO C3 field of view. We also obtain power-law functions for both CME mean density at 21 solar radii and ICME mean density at 1AU, with the average power-law index of 2.6. We estimate a ratio of CME density to background density based on the Leblanc et al.(1998) at 21 solar radii. Interestingly, the average of the ratios is 4.0, which is the same as a default value used in the WSA-ENLIL model.

• Journal of Astronomy and Space Sciences
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• 제12권2호
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• pp.157-167
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• 1995

OH/IR stars are the most massive and youngest subclass in asymptotic giant branch stars which pass through sporadic superwind phases. We have modeled the dust envelopes around OH/IR stars with close attention to the evolution of the structure of the dust shells. We use various dust density distributions to take account the effect of the superwind due to the helium shell flash by adding a density increased region. Depending on the position and quality of the density increased region, the model results are different from the results with conventional density distribution. The new results fit the observations of some OH/IR stars better. Especially, the OH/IR stars with excessive 30-100$\mu$m emission can be better explained by the new results. The IR two-color diagrams comparing the results of the superwind models and IRAS observation of 95 OH/IR stars have been made. The new results can explain much wider regions on the IR two-color diagrams.

• Journal of Astronomy and Space Sciences
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• 제39권3호
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• pp.87-98
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• 2022

The Far-UltraViolet (FUV) imager onboard the Ionospheric Connection Explorer (ICON) spacecraft provides two-dimensional limb images of oxygen airglow in the nightside low-latitude ionosphere that are used to determine the oxygen ion density. As yet, no FUV limb imager has been used for climatological analyses of Equatorial Plasma Bubbles (EPBs). To examine the potential of ICON/FUV for this purpose, we statistically investigate small-scale (~180 km) fluctuations of oxygen ion density in its limb images. The seasonal-longitudinal variations of the fluctuation level reasonably conform to the EPB statistics in existing literature. To further validate the ICON/FUV data quality, we also inspect climatology of the ambient (unfiltered) nightside oxygen ion density. The ambient density exhibits (1) the well-known zonal wavenumber-4 signatures in the Equatorial Ionization Anomaly (EIA) and (2) off-equatorial enhancement above the Caribbean, both of which agree with previous studies. Merits of ICON/FUV observations over other conventional data sets are discussed in this paper. Furthermore, we suggest possible directions of future work, e.g., synergy between ICON/FUV and the Global-scale Observations of the Limb and Disk (GOLD) mission.

• Journal of Astronomy and Space Sciences
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• 제10권2호
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• pp.163-188
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• 1993

적색편이 공간에서 보이는 국부 요동지역 주변의 초면은 프리이드만 배경 우주에 포함된 툴만 시공간 모형 관점에서 보면 국부 중력장에 유도된 국부 팽창율이 원인이 됨을 알고 있다. 초면은 국부적인 것으로서 요동지역에 포함된 질량에 크게 지배되고 물질들의 동력학적 상태와 밀접한 관계가 았다. 은하단의 밀도 분포 모형으로 광학 관측과 X-선 관측을 잘 맞추는 아벨 윤곽과 폴리트로프적 밀도 분포 윤곽을 택하여 틀만 시공간 모형으로 계산한 적색편이 공간에 나타나는 초면과 코마 은하단과 페르세우스 은하단 성분은하들에서 관측되는 적색편이-중심거리 형태와 비교하였을 때, 초면은 은하단의 크기와 질량에 한계값을 설정할 수 있었고, 뜨거운 기체의 물질 상태를 짐작할 수 있는 단서를 제공한다.

• 한국멀티미디어학회논문지
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• 제9권6호
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• pp.728-734
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• 2006

Carrier interferometry code is considered as a promising scheme that provides significant performance improvement via frequency diversity effect. Space-time coding is commonly employed to achieve a performance gain through space diversity. The combination of these techniques and forward error correction coding will lead to enhanced system capacity and performance. This paper presents a low-density parity check (LDPC) coded space-time orthogonal frequency division multiplexing (OFDM) transmission scheme with carrier interferometry code for high-capacity and high-performance mobile multimedia communications. Computer simulations demonstrate that the proposed mobile multimedia transmission system offers a considerable performance improvement of approximately 9dB in terms of Eb/No in the Rayleigh fading channel with relatively low delay spread, in comparison with space-time OFDM. Performance gains are further increased, comparing with traditional OFDM systems.