• Bulletin of the Korean Space Science Society
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• 2003.10a
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• pp.38-38
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• 2003

전리층은 우주환경의 변화에 매우 중요한 역할을 하고 있다. 그 중 전리층에서 발생하는 오로라는 우주환경의 변화를 가시적으로 보여주는 유일한 현상이다. 본 연구에서는 오로라 타원체를 따라 흐르는 오로라 제트전류의 위도에 따른 분포를 알아보고 그 특징을 조사하였다. 그리고 오로라 발생지역과 이들 전류분포를 비교하였으며 전기장과 전기전도도를 계산하여 오로라 제트전류에 대한 상대적인 기여도를 알아보았다. 먼저 CANOPUS 지자기 관측소의 1998년 데이터를 사용하여 1년간 발생했던 Isolated Substorm을 추려내었다. 그리고 이들 Substorm이 발생하는 동안 위도에 따른 오로라 제트전류 분포의 특징을 구하여 전류의 방향에 따라 이들 분포가 어떠한 형태로 나타나는지 알아보았으며, 이때 오로라 발생지역과의 연관성을 조사하였다. 여기서 전리층에 흐르는 전류를 무한판상으로 가정하여 오로라 제트전류의 분포를 지자기변화 성분으로부터 추론하였다. 또한 DMSP의 하강입자를 이용하여 계산한 전기전도도를 이용해 전기장을 추정함과 동시에 오로라제트전류에 대한 이들의 상대적 기여도를 조사해보았다.

• Bulletin of the Korean Space Science Society
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• 2004.10b
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• pp.380-383
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• 2004

We study the two storm events of 1997: one in May that was accompanied by a relativistic electron event (REE) and the other in September, with a more profound Dst decrease, but with no significant flux increase of relativistic electrons. We find that a larger amount of seed electrons was present in the May event compared to that of the September storm, whereas the ULF (ultra low frequency) power was more enhanced and the particle spectrum was harder in the September event. Hence, we demonstrate that a larger storm does not necessarily produce more seed electrons and that the amount of seed electrons is an important factor in an actual increase in REE flux levels, while ULF can harden the particle spectra without causing an apparent REE.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.1
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• pp.33.1-33.1
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• 2011

The plasma sheet of the Earth's magnetosphere is a sheet of hot plasmas in the magnetotail region, dividing the two (northern and southern) lobes of the Earth's magnetic field. It is the key region that is often closely linked to various electromagnetic dynamics in the Earth's magnetosphere-ionosphere system. In particular, it is the region that is most crucial for substorms, which is one of the most dynamic phenomena in the Earth's magnetosphere. The question of substorm triggering remains highly controversial until today, and at the center of the controversy there are several critical physics issues of the plasma sheet. In this talk I will introduce some of the physics issues of the plasma sheet. The specific topics that this talk will cover are (i) the general properties of the plasma sheet, (ii) fast plasma jets and plasma transport problem, (iii) stability/instability problem, and (iv) effects of thin current sheet. I will also present some of our group's recent findings regarding these topics, as obtained by comprehensive analyses of various observational data. The level and content of this talk are designed to be comprehensible to not only space physicists but also the scientists in a related field such as solar and heliospheric physics.

• Bulletin of the Korean Space Science Society
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• 2003.05b
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• pp.68-68
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• 2003

• Bulletin of the Korean Space Science Society
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• 2001.11a
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• pp.43-43
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• 2001

• Bulletin of the Korean Space Science Society
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• 2003.05b
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• pp.43-43
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• 2003

No Abstract, See Full Text

• Journal of Astronomy and Space Sciences
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• v.20 no.1
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• pp.43-52
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• 2003

This paper reports a statistical study on the relationship between relativistic electron events(REE), magnetic storms, and substorms. We have used magnetic storm events that occurred between 1996 and 1998, and have classified them into two groups, (i) magnetic storms with REE and (ii) magnetic storms without REE, according to whether or not the magnetic storm is accompanied by REE. Then we have examined the characteristics of substorms that occurred during the main phase of each of the magnetic storms, and compared them between the two groups of the storms. In particular, we have made some quantitative estimations on the intensities of the energetic particle injections and magnetic dipolarizations during the substorm. We find that the injection intensity ratio and the magnetic dipolaization of the storm-time substorms are bigger for substorms with REE than for those without REE.

• Bulletin of the Korean Space Science Society
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• 2008.04a
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• pp.24.2-24.2
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• 2008

• Bulletin of the Korean Space Science Society
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• 2007.10a
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• pp.42-42
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• 2007

• Bulletin of the Korean Space Science Society
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• 2003.10a
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• pp.40-40
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• 2003

When the magnetotail is disturbed by an impulsive input such as the substorm onset, compressional magnetohydrodynamic (MHD) waves play an important role in delivering perturbed energy and exciting various wave modes and currents. The plasmasheet, in which relatively hot plasmas exist, is surrounded by relatively cold plasmas at the plasma sheet boundary layer (PSBL) and the equatorial plasmasphere. Since the Alfven speed significantly varies near these regions, the compressional waves are expected to undergo mode conversion by inhomogeneity at the boundary between cold and hot plasma regions. We investigate how the initial compressional MHD wave energy is reflected, transmitted, and absorbed across that boundary by adopting the invariant imbedding method (IIM) which gives the exact reflection, transmission, and absorption coefficients without any theoretical approximations for given frequencies and wave numbers. The IIM method is very useful in quantifying the reflection and transmission of compressional waves in the sense that we can calculate how much fast mode wave energy is delievered into shear Alfven waves or field-aligned currents. Our results show that strongly localized absorption occurs at the boundary region. This feature suggests that localized field-aligned currents can be impulsively excited at such boundary regions by any compressional disturbances, which is highly associated with impulsive auroral brightening at the substorm onset. We compare our results with previous studies in cold inhomogeneous plasmas.