• Proceedings of the Korean Magnestics Society Conference
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• 2011.12a
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• pp.21-22
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• 2011

• Proceedings of the Korean Magnestics Society Conference
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• 2012.05a
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• pp.61-62
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• 2012

• Journal of the Korean Magnetics Society
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• v.22 no.6
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• pp.200-203
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• 2012

In this study, we have investigated that the operation frequency dependences of the output properties of the orthogonal fluxgate sensor which was fabricated with a ferrite core. An orthogonal fluxgate sensor should be operated in as high as possible frequency to enhance its sensitivity in the case of small sized sensor, because sensitivity of the sensor is proportional to cross section area, winding number and operation frequency. In this study, we investigated the correspondence of the frequency dependence of output and the reactance (inductance and capacitance) of pickup coil and cable. Experimental results represented that we could obtain maximum output (= sensitivity) at optimal frequency which is near LC resonance frequency of the pickup coil and cable.

• Journal of Astronomy and Space Sciences
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• v.20 no.2
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• pp.109-122
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• 2003

To examine the causal relationship between geomagnetic storm and substorm, we investigate the correlation between dispersionless particle injection rate of proton flux observed from geosynchronous satellites, which is known to be a typical indicator of the substorm expansion activity, and Dst index during magnetic storms. We utilize geomagnetic storms occurred during the period of 1996 ~ 2000 and categorize them into three classes in terms of the minimum value of the Dst index ($Dst_{min}$); intense ($-200nT{$\leq$}Dst_{min}{$\leq$}-100nT$), moderate($-100nT{\leq}Dst_{min}{\leq}-50nT$), and small ($-50nT{\leq}Dst_{min}{\leq}-30nT$) -30nT)storms. We use the proton flux of the energy range from 50 keV to 670 keV, the major constituents of the ring current particles, observed from the LANL geosynchronous satellites located within the local time sector from 18:00 MLT to 04:00 MLT. We also examine the flux ratio ($f_{max}/f_{ave}$) to estimate particle energy injection rate into the inner magnetosphere, with $f_{ave}$ and $f_{max}$ being the flux levels during quiet and onset levels, respectively. The total energy injection rate into the inner magnetosphere can not be estimated from particle measurements by one or two satellites. However, the total energy injection rate should be at least proportional to the flux ratio and the injection frequency. Thus we propose a quantity, “total energy injection parameter (TEIP)”, defined by the product of the flux ratio and the injection frequency as an indicator of the injected energy into the inner magnetosphere. To investigate the phase dependence of the substorm contribution to the development of magnetic storm, we examine the correlations during the two intervals, main and recovery phase of storm separately. Several interesting tendencies are noted particularly during the main phase of storm. First, the average particle injection frequency tends to increase with the storm size with the correlation coefficient being 0.83. Second, the flux ratio ($f_{max}/f_{ave}$) tends to be higher during large storms. The correlation coefficient between $Dst_{min}$ and the flux ratio is generally high, for example, 0.74 for the 75~113 keV energy channel. Third, it is also worth mentioning that there is a high correlation between the TEIP and $Dst_{min}$ with the highest coefficient (0.80) being recorded for the energy channel of 75~113 keV, the typical particle energies of the ring current belt. Fourth, the particle injection during the recovery phase tends to make the storms longer. It is particularly the case for intense storms. These characteristics observed during the main phase of the magnetic storm indicate that substorm expansion activity is closely associated with the development of mangetic storm.

• Electrical & Electronic Materials
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• v.14 no.5
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• pp.16-24
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• 2001

• Journal of the Korean Magnetics Society
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• v.19 no.1
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• pp.17-21
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• 2009

In this study, we have investigated that the excitation current and operation frequency dependences of the output properties of the orthogonal fluxgate sensor which was fabricated with a Co base amorphous wire and a pick-up coil. The output signal increased linearly with increase of the excitation current below 0.3 A, and decreased with increase of the excitation current over 0.6 A. It was also found that the output increased sensitively with increase of operation frequency below 1.3MHz. The output was 3.8 V at the frequency of 1.3MHz while 1.32 V at 1MHz.

• Journal of Space Technology and Applications
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• v.2 no.3
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• pp.221-229
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• 2022

This paper reports on the design and installation of a thermostat to keep the temperature of the fluxgate magnetometer constant and the data stability evaluation after installation. The thermostat was installed at the Icheon Geomagnetic Observatory operated by the Korean Space Weather Center of National Radio Research Agency. It was designed in consideration of stability of temperature control against safety incident, potential effects on magnetic field measurement, and the temperature control efficiency. After the temperature control device was installed, it was confirmed that the temperature was constantly maintained at the level of 20℃. Delta F and baseline values were used to evaluate geomagnetic data stability, and it was confirmed that delta F and baseline fluctuations were reduced after installation of the thermostat.

• Proceedings of the Korean Magnestics Society Conference
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• 1993.11a
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• pp.26-27
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• 1993

• Proceedings of the Korean Magnestics Society Conference
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• 2012.11a
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• pp.46-47
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• 2012

• The Bulletin of The Korean Astronomical Society
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• v.35 no.2
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• pp.47.2-47.2
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• 2010

태양플레어는 태양 대기에서 발생하는 격렬한 폭발현상으로 이를 예측하고 대비하기가 쉽지 않다. 본 연구에서는 플레어의 발생 확률이 태양 흑점 분류와 흑점 면적 변화량에 어떻게 의존하는 가를 조사하였다. 이를 위하여 약 9년 기간(2001년 7월 ~ 2010년 6월) NOAA에서 제공하는 AR(Active Region) 정보에 근거한 McIntosh 흑점 분류법을 사용하였다. 플레어는 C 등급 이상(C,M,X)인 것만을 고려하였다. 본 연구에서는 60개의 McIntosh 흑점군 그룹 중 가장 플레어를 많이 발생시키는 6개의 흑점군 그룹에 대해 태양 흑점 면적의 변화량을 각각 3그룹으로 나누어(감소, 무변화, 증가) 비교해보았다. 그 결과 거의 모든 그룹에서 태양 흑점의 넓이가 증가, 감소, 무변화 순으로 플레어의 발생 확률이 높다는 것을 확인하였다. 예로, 흑점군 그룹 중 Fkc그룹의 경우 위의 순서대로 65%, 50%, 44%로 M등급의 플레어가 발생했다. 흑점의 면적 변화가 자기플럭스의 변화를 나타내는 좋은 인자임을 고려할 때, 본 결과는 새로운 자기플럭스가 광구로 상승하는 경우에 플레어의 발생 확률이 더 높음을 보여준다. 본 연구 결과를 토대로 태양 흑점 분류와 면적의 변화량에 따른 플레어 발생 확률 연구의 발전방향과 활용 방안에 대해 논의하고자 한다.