• Bulletin of the Korean Space Science Society
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• 2003.10a
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• pp.80-80
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• 2003

서브스톰이 진행될 때 극지방의 지자기 교란은 대류 제트 전류와 서브스톰 전류 쐐기로 구성되는 오로라 제트 전류에 기인한다. 이들은 전기장 강화를 뜻하는 AU 지수와 전기 전도도 강화를 뜻하는 AL 지수로 나타낼 수 있다. 이들 AU, AL 지수와 자기폭풍의 정도를 나타내는 Dst 지수와의 상관관계를 구해봄으로써 서브스톰이 자기폭풍의 형성에 어떻게 기여하는지 조사하였다. 이를 위하여 월별 누적 AU, 누적 │AL│ 값을 구한 뒤 월별 누적 Dst 와의 상관관계를 구하였다. 한편 IMF(Interplanetary Magnetic Field)의 남쪽 자기장 성분으로부터 지구 자기장 내에 강력한 전기장이 형성되어 자기폭풍을 형성한다는 견해가 있다. 전기장 E=V(태양풍 속도)$\times$Bs(IMF의 남쪽 자기장 성분)으로 나타낼 수 있으므로 이로부터 구한 월별 누적 전기장과 누적 Dst 값을 비교해 봄으로써 자기권 대류가 자기폭풍 형성에 어느 정도 기여하는지 조사하였다. 본 연구를 위하여 1966년부터 1987년까지 20년간의 AE(AU, AL) 지수를 이용하였으며 IMF 자료는 ACE 위성이 제공하는 행성간 자기장 자료로 1997년부터 2002년까지의 자료를 이용하였다. 본 연구의 결과는 현재 논쟁이 되고 있는 storm-substorm의 인과관계를 보다 잘 규명할 것으로 기대된다.

• The Bulletin of The Korean Astronomical Society
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• v.25 no.1
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• pp.19-19
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• 2000

• Proceedings of the Korean Institute of Navigation and Port Research Conference
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• 2013.06a
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• pp.111-112
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• 2013

GPS는 항행, 측량, 지도제작, 시각동기 등 정확한 위치정보가 필요한 여러 분야에서 활용되고 있으며, 이에 대한 의존도는 점점 증가하고 있는 추세이다. 따라서 GPS 신호에 이상이 발생하는 경우 GPS를 기반으로 한 여러 시스템에서 혼란 및 막대한 경제적 손실이 발생할 것으로 예상된다. 이를 방지하기 위해 GPS 신호의 이상 감시를 위한 연구가 활발히 이루어지고 있는 추세이며, 이러한 연구 중에는 기존의 이상사례에 대해 분석하는 부분도 포함된다. GPS 신호 이상은 위성 고장, 태양폭풍에 의한 이온층의 급격한 변화, 항법메시지의 오류, 전자파 간섭 등 여러 요인에 의해 발생하게 된다. 본 논문에서는 위성 고장 사례 중 위성시계 이상, 위성궤도 이상와 이온층 폭풍에 의한 이상, 대류층 변화에 의한 이상에 대해 분석하고 이 때 고장으로 인해 발생한 이상신호에 대해 모델링을 수행한다. 기존의 이상사례에 대한 분석결과 및 모델링한 신호는 GPS 신호의 이상 감시 알고리즘을 개발 및 검증하기 위한 목적으로 활용될 수 있을 것으로 기대된다.

• Bulletin of the Korean Space Science Society
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• 2006.10a
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• pp.54-54
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• 2006

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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• pp.213.1-213.1
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• 2012

우주방사선폭풍탐사선 (Space Radiation Storm probe: SRSP)에 탑재할 과학측정 장비들 중의 하나로 추진 중인 PD는 우주방사선 환경에서의 태양활동에 따른 고에너지 하전입자들 특히 proton의 에너지와 flux에 대한 정보를 획득하고 더불어 다른 고에너지 입자의 효과까지 포함하는 Linear Energy Transfer (LET)을 측정하기 위한 탑재체이다. 본 연구팀은 PD의 사양을 결정하기 위해서 GEANT4를 사용하여 전산모사를 수행하였으며, proton의 경우 우주 방사선 환경에서의 태양활동에 따른 고에너지 영역을 고려하여 0.1 ~ 1000 MeV 범위에서 전산 모사를 수행하였다. 본 연구팀은 특히 PD의 에너지 범위를 0 MeV ~ 5 MeV, 5 MeV ~ 10 MeV, 10 MeV ~ 20 MeV, 20 MeV ~ 35 MeV, 35 MeV ~ 52 MeV, 52 MeV ~ 72 MeV, 72 MeV 이상으로 총 7개의 channel를 결정하고 Al의 blocking material을 사용하여 검출하려는 에너지 범위를 조절한다. 또한 최적의 채널을 결정하여 silicon detector를 사용한 탑재체의 개념 설계를 실시하였다. 설계된 PD로부터 방사선대에서의 proton를 측정함으로써 태양기원 고에너지 입자에 대한 포획 및 쇠퇴에 대한 이해를 도울 것이다.

• Aerospace Engineering and Technology
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• v.12 no.2
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• pp.99-107
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• 2013

Local dust storm and lifting to dust frequently occurs in Mars. But it is known to lift dust is associated with atmospheric circulation, the cause of dust lifting is not find yet. The height of dust storm is more than the Himalayas, and the large size dust storm covers half of hemisphere or hemisphere. The kind of dust storm is risk factor to land and to carry out a mission. In this paper, we carry out analysis on the season and place of dust storm, and construct a map with the place of dust storm. We expect that the season and place of dust storm are able to be predicted with being based on the results. And this paper can be utilized as preliminary for selection of landing site and time of launching and landing.

• Journal of Astronomy and Space Sciences
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• v.25 no.2
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• pp.157-166
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• 2008

We have investigated a statistical relationship between sawtooth oscillations and geomagnetic storms during 2000-2004. First of all we selected a total of 154 geomagnetic storms based on the Dst index, and distinguished between different drivers such as Coronal Mass Ejection (CME) and Co-rotating Interaction Region (CIR). Also, we identified a total of 48 sawtooth oscillation events based on geosynchronous energetic particle data for the same 2000-2004 period. We found that out of the 154 storms identified, 47 storms indicated the presence of sawtooth oscillations. Also, all but one sawtooth event identified occurred during a geomagnetic storm interval. It was also found that sawtooth oscillation events occur more frequently for storms driven by CME $({\sim}62%)$ than for storms driven by CIR $({\sim}30%)$. In addition, sawtooth oscillations occurred mainly $({\sim}82%)$ in the main phase of storms for CME-driven storms while they occurred mostly $({\sim}78%)$ during the storm recovery phase for CIR-driven storms. Next we have examined the average characteristics of the Bz component of IMF, and solar wind speed, which were the main components for driving geomagnetic storm. We found that for most of the sawtooth events, the IMF Bz corresponds to -15 to 0 nT and the solar wind speed was in the range of $400{\sim}700km/s$. We found that there was a weak tendency that the number of teeth for a given sawtooth event interval was proportional to the southward IMF Bz magnitude.

• Journal of Satellite, Information and Communications
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• v.6 no.2
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• pp.107-111
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• 2011

In World War II, the solar eruption (solar flare) was revealed to make a significant effect to radar systems. The radio disturbance in February 28, 1942 was due to increased cosmic ray during solar maximum. Since such phenomena had been disclosed, many studies were accomplished on solar flare and solar particle event. Now various researches about the effects of solar flare on the spacecrafts, the airplanes flying across the pole, the radar systems, and wireless communication systems are studied. In this paper we analyzed the relationship between the harmful effect on the wireless communication by the solar eruption and the period of solar activity from the sunspot number data and the solar radio burst data for last 40 years.

• Journal of the Korean Society of Surveying, Geodesy, Photogrammetry and Cartography
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• v.29 no.6
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• pp.651-657
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• 2011

There exists a high correlation between the ionospheric delays and the integer ambiguity in GPS observation equation, so that the sufficient time span is required to revolve the integer ambiguity. This means that the ambiguity resolution plays a key role especially in rapid-static positioning mode. To analyze the effect of ionospheric disturbances on the positioning accuracy, 02/19/2011 day of dataset was selected processed in rapid-static positioning mode. The total of 141 30-minute sessions were processed, i.e., the estimation procedure started every 10 minutes, and the time-to-fix information of each data interval is obtained. In this study, the analysis is performed by comparing the time-to-fix with the magnitudes of ionospheric delays. The computed correlation coefficient between the time-to-fix and the magnitudes of ionospheric delays is 0.31, which indicates the ionospheric disturbances affect the positioning accuracy in rapid-static positioning mode. Therefore, it is required to collect and process sufficient data when the GPS surveying is performed in unfavorable ionospheric conditions.

• Journal of Astronomy and Space Sciences
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• v.24 no.2
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• pp.125-134
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• 2007

In this paper, we analyze the orbital variation of the Korea Multi-Purpose SATellite-1(KOMPSAT-1) in a strong space environment due to satellite drag by solar and geomagnetic activities. The satellite drag usually occurs slowly, but becomes serious satellite drag when the space environment suddenly changes via strong solar activity like a big flare eruption or coronal mass ejections(CMEs). Especially, KOMPSAT-1 as a low earth orbit satellite has a distinct increase of the drag acceleration by the variations of atmospheric friction. We consider factors of solar activity to have serious effects on the satellite drag from two points of view. One is an effect of high energy radiation when the flare occurs in the Sun. This radiation heats and expands the upper atmosphere of the Earth as the number of neutral particles is suddenly increased. The other is an effect of Joule and precipitating particle heating caused by current of plasma and precipitation of particles during geomagnetic storms by CMEs. It also affects the density of neutral particles by heating the upper atmo-sphere. We investigate the satellite drag acceleration associated with the two factors for five events selected based on solar and geomagnetic data from 2001 to 2002. The major results can be summarized as follows. First, the drag acceleration started to increase with solar EUV radiation with the best cross-correlation (r = 0.92) for 1 day delayed F10.7. Second, the drag acceleration and Dst index have similar patterns when the geomagnetic storm is dominant and the drag acceleration abruptly increases during the strong geomagnetic storm. Third, the background variation of the drag accelerations is governed by the solar radiation, while their short term (less than a day) variations is governed by geomagnetic storms.