• 천문학회지
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• 제38권4호
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• pp.463-470
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• 2005

In this paper, we have made the component-based development of observational software for KASI solar imaging spectrograph (KSIS) that is able to obtain three-dimensional imaging spectrograms by using a scanning mirror in front of the spectrograph slit. Since 2002, the KASI solar spectrograph has been successfully operated to observe solar spectra for a given slit region as well as to inspect the response functions of narrow band filters. To improve its capability, we have developed the KSIS that can perform sequential observations of solar spectra by simultaneously controlling the scanning mirror and the CCD camera via Visual C++. Main task of this paper is to introduce the development of the component-based software for KSIS. Each component of the software is reusable on the level of executable file instead of source code because the software was developed by using CBD (component-based development) methodology. The main advantage of such a component-based software is that key components such as image processing component and display component can be applied to other similar observational software without any modifications. Using this software, we have successfully obtained solar imaging spectra of an active region (AR 10708) including a small sunspot. Finally, we present solar $H{\alpha}$ spectra ($6562.81{\AA}$) that were obtained at an active region and a quiet region in order to confirm the validity of the developed KSIS and its software.

• 천문학회보
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• 제35권2호
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• pp.46.1-46.1
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• 2010

This work is a part of our project to establish a Website which provides a list of magnetic clouds (MCs) identified by WIND and ACE spacecraft. MCs are characterized by their magnetic fields that are well described by magnetic flux rope structures, whereas interplanetary coronal mass ejections (ICMEs) are interplanetary manifestations of coronal mass ejections (CMEs), usually identified by differences of plasma and magnetic field characteristics from those in the background solar wind. It is widely accepted that, while MCs are generally identified within ICMEs, the number of MCs are significantly lower than the number of ICMEs. In our effort to identify MCs, however, we have found that there was a big problem in identification method of MCs in previous works. Generally speaking, most of the previous surveys failed in identifying MCs which encounter the spacecraft at large distances from the MC axis, or near the surface of MC structures. In our survey, MCs are identified as the region of which magnetic fields are well described by appropriate flux rope models. Thus, we could selected over 45 MCs, in 1999 solar wind data for instance, while 33 ICMEs are listed in the Website of the ACE Science Center reported by Richardson and Cane.

• 한국컴퓨터정보학회논문지
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• 제23권4호
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• pp.139-145
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• 2018

In this paper, we propose the methodology and system to show weather information to spatial system. When using the spatial information system, it is easy and convenient to show information such as target location, mission contents, enemy threats and so on. However, drawing 1-dimensional weather information on 3-dimensional space in spatial information system is hard task. To fuse data, we need to add a spatial layer including weather information to spatial layers and perform space modeling for showing weather information as spatial data in a virtual space. The virtual space is shown by receiving meteorological data and then changing in real time through weather database linkage.

• 천문학회보
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• 제35권2호
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• pp.45.2-45.2
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• 2010

We analyzed onset times of the largest six solar proton events during 1997-2006 of solar cycle 23, as observed at 1AU by two satellites of GOES/SEM (Geostationary Operational Environmental Satellites/the Space Environment Monitor) and SOHO/ERNE (Solar and Heliospheric Observatory/the Energetic and Relativistic Nuclei and Electron). We adopted the time shifted method suggested by Leon Kocharov and determined the path length by Sam Krucker's fitting method. We found some problems of those methods and tried to improve those. In this presentation, we will give details of the energy spectra of the 6 SPE events from the ERNE/HED, and onset time comparison among the SPE, flare, type II burst, and CME.

• 천문학회보
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• 제34권1호
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• pp.81.2-81.2
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• 2009

• 한국항행학회논문지
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• 제26권5호
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• pp.350-357
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• 2022

최근 'Cycle 25'의 태양 활동 극대기가 다시 도래함에 따라 우주기상 연구에 대한 중요성이 높아지고 있다. 이에 WRC(World Radiocommunication Conference)-23에서는 의제 9.1a)를 채택하여 능동/수동 우주기상 관측시스템과 기존 업무와의 주파수 공유 연구 결과를 검토해 나가고 있다. 따라서 본 논문에서는 우주기상 환경 데이터의 정밀도를 높이고 관측 서비스의 주파수 스펙트럼 확보를 위해 제주 고산 기상 레이더로부터 제주 한림의 우주기상 관측 수신기에 미치는 직접 간섭영향과 레이더 목표물에서의 회절 및 산란에 의해 관측 수신기에 미치는 간접 간섭영향을 분석하였다. 분석 결과 레이더 방향 및 목표물로부터 회절 및 산란되는 전파 방향, 레이더 목표물의 RCS(radar cross section), 우주기상 관측 안테나의 수신 면적 및 오프 보어 사이트(off-boresight) 등이 간섭 영향 분석에 중요 파라미터임을 알 수 있다.

• 천문학회보
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• 제40권1호
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• pp.64.4-65
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• 2015

For the past decade, supported by the Korean government, the solar and space weather group of Korea Astronomy and Space Science Institute (KASI) has been researching towards the prevention of hazardous effects on Korean satellites, the stability of wireless telecommunications, and the safety of polar route aviation. So far, we have expanded the ground observation system, made space data more accessible, developed more advanced models for space weather forecasting, from which we have been providing forecasting services to a satisfied domestic clientele. Alongside that, we have continued our research on solar activities and the Sun-Earth connection. In this talk, I will summarize our contributions to space weather over the past 10 years and discuss future plans for next decade.

• 천문학회보
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• 제42권2호
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• pp.62.3-63
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• 2017

The Mars Atmosphere and Volatile (MAVEN) mission has been providing valuable information on the atmospheric loss of Mars since its launch in November 2013. The Neutral Gass and Ion Mass Spectrometer (NGIMS) onboard MAVEN, was developed to analyze the composition of the Martian upper atmospheric neutrals and ions depending on various space weather conditions. We investigate a variation of upper atmospheric ion densities depending on the interplanetary coronal mass ejections (ICMEs). It is known that the Mars has a very weak global magnetic field, so upper atmosphere of Mars has been strongly affected by the solar activities. Meanwhile, a strong crustal magnetic field exists on local surfaces, so they also have a compensating effect on the upper atmospheric loss outside the Mars. The weak crustal field has an influence up to 200km altitude, but on a strong field region, especially east longitude of $180^{\circ}$ and latitude of $-50^{\circ}$, they have an influence over 1,400km altitude. In this paper, we investigated which is more dominant between the crustal field effect and the ICME effect to the atmospheric loss. At 400km altitude, the ion density over the strong crustal field region did not show a significant variation despite of ICME event. However, over the other areas, the variation associated with ICME event is far more overwhelming.

• Journal of Astronomy and Space Sciences
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• 제29권4호
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• pp.397-405
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• 2012

Astronomical Observations at Chungbuk National University Observatory (CBNUO) with an 1 m telescope have begun since April 2008, and Near-Earth Space Survey observations also have been started since November 2010, with a 0.6 m wide field telescope developed by Korea Astronomy and Space Science Institute. To improve observational efficiency, we developed a weather monitoring system enabling automatic monitoring for the weather conditions and checking the status of the observational circumstances, such as dome status. We hope this weather monitoring system can be helpful to more than 100 Korean domestic observatories, including public outreach facilities. In this paper, we present the statistic analysis of the weather conditions collected at CBNUO for 3 years (2009- 2011) and comparisons were made for clear nights between using only humidity data and both humidity and cloud data.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2004년도 한국우주과학회보 제13권1호
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• pp.37-37
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• 2004

It is well known that solar activity such as coronal mass ejections(CMEs) and flares is a direct driver of space weather. In this talk, we introduce its main physical characteristics and physical connections among CMEs(or flares) -Interplanetary(IP) shocks - interplanetary CMEs (or magnetic clouds) - geomagnetic storms. Specifically, solar activity is discussed in terms of space weather scales (R:Radio Blackout, S: Solar Radiation Storms, G: Geomagnetic Storms). (omitted)