• 한국재난정보학회:학술대회논문집
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• 한국재난정보학회 2023년 정기학술대회 논문집
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• pp.221-221
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• 2023

1969년에 발간된 API521 1st edition에서는 Flare Load 저감용으로 적용되는 HIPS (High Integrity Protection System)는 모두 Pressure Safety Valve의 고장확률보다 낮은 SIL 3 (Safety Integrity Level)등급을 적용할 것을 요구하고 있다. Flare Stack 저감용 HIPS는 주로 압축기 출력압력상승, Reboiler Steam 과다주입, 전력공급중단냉각펌프고장 등에 의한 Flare 발생을 예방하기 위한 기능을 가진 SIF (Safety Instrumented Function)로 구성된다. 하지만 2007년도 발간된 API521 5th edition에서는 LOPA (Layer Of Protection Analysis) 분석을 통해 Target SIL을 도출하는 것으로 요구사항을 변경했다. 이에 따라 이번 연구에서는 Flare Load에 가장 큰 영향을 미치는 시나리오 중 대표적인 시나리오를 대상으로 HAZOP(Hazard and Operability Study)과 LOPA분석을 실시해서 Target SIL이 어떻게 도출되는지를 연구했다. Flare Stack에서 Flare를 발생시키는 대표적인 시나리오들에 대해 LOPA분석을 실시한 결과 압축기 출력압력상승은 SIL 2, Reboiler Steam 과다주입은 SIL 3, 전력공급중단은 SIL 0, 냉각펌프고장은 SIL 0로 모두가 SIL 3 가 나오지는 않았다. SIF 설계 시 Target SIL을 만족시키는 것도 중요하지만 운전 시 SIL 등급이 계속 유지되게 하지 위해 인적오류, 시스템적 고장, 하드웨어고장 등에 의해 SIF 기능불능화가 되는 것을 예방하기 위한 기능안전관리시스템 (FSMS)를 적용하는 것도 중요하다.

• 천문학회보
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• 제37권2호
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• pp.123.2-123.2
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• 2012

We investigate the solar flare occurrence rate and daily flare probability in terms of the sunspot classification supplemented with sunspot area and its changes. For this we use the NOAA active region data and GOES solar flare data for 15 years (from January 1996 to December 2010). We consider the most flare-productive eleven sunspot classes in the McIntosh sunspot group classification. Sunspot area and its changes can be a proxy of magnetic flux and its emergence/cancellation, respectively. We classify each sunspot group into two sub-groups by its area: "Large" and "Small". In addition, for each group, we classify it into three sub-groups according to sunspot area changes: "Decrease", "Steady", and "Increase". As a result, in the case of compact groups, their flare occurrence rates and daily flare probabilities noticeably increase with sunspot group area. We also find that the flare occurrence rates and daily flare probabilities for the "Increase" sub-groups are noticeably higher than those for the other sub-groups. In case of the (M+X)-class flares in the 'Dkc' group, the flare occurrence rate of the "Increase" sub-group is three times higher than that of the "Steady" sub-group. Our results statistically demonstrate that magnetic flux and its emergence enhance the occurrence of major solar flares.

• 천문학회보
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• 제41권2호
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• pp.42.1-42.1
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• 2016

The formation process and the dynamical properties of a large-scale quasi-circular flare ribbon were investigated using the SDO AIA and HMI data along with data from RHESSI and SOT. Within one hour time interval, two subsequent M-class flares were detected from the NOAA 12371 that had a ${\beta}{\gamma}{\delta}$ configuration with one bipolar sunspot group in the east and one unipolar spot in the west embedded in a decayed magnetic field. Earlier M2.0 flare was associated with a coronal loop eruption, and a two-ribbon structure formed within the bipolar sunspot group. On the other hand, the later M2.6 flare was associated with a halo CME, and a quasi-circular ribbon developed encircling the full active region. The observed quasi-circular ribbon was strikingly large in size spanning 650" in north-south and 500" in east-west direction. It showed the well-known sequential brightening in the clockwise direction during the decay phase of the M2.6 flare at the estimated speed of 160.7 km s-1. The quasi-circular ribbon also showed the radial expansion, especially in the southern part. Interestingly, at the time of the later M2.6 flare, the third flare ribbon parallel to the early two-ribbon structure also developed near the unipolar sunspot, then showed a typical separation in pair with the eastern most ribbon of the early two ribbons. The potential field reconstruction based on the PFSS model showed a fan shaped magnetic configuration including fan-like field lines stemming from the unipolar spot and fanning out toward the background decayed field. This large-scale fan-like field overarched full active region, and the footpoints of fan-like field lines were co-spatial with the observed quasi-circular ribbon. From the NLFF magnetic field reconstruction, we confirmed the existence of a twisted flux rope structure in the bipolar spot group before the first M2.0 flare. Hard X-ray emission signatures were detected at the site of twisted flux rope during the pre-flare phase of the M2.0 flare. Based on the analysis of both two-ribbon structure and quasi-circular ribbon, we suggest that a tether-cutting reconnection between sheared arcade overarching the twisted flux rope embedded in a fan-like magnetic field may have triggered the first M2.0 flare, then secondary M2.6 flare was introduced by the fan-spine reconnection because of the interaction between the expanding field and the nearby quasi-null and formed the observed large-scale quasi-circular flare ribbon.

• 천문학회보
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• 제40권1호
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• pp.63.2-63.2
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• 2015

Solar flare is one of the energetic phenomena observed on the Sun, and it is often accompanied with eruptions such as global-scale eruption of a flux rope (filament/prominence eruption) and small-scale eruption of a plasmoid. A flare itself is a dissipative phenomenon where accumulated electric current representing free magnetic energy is dissipated quickly at a special location called a current sheet formed in a generally highly conductive solar corona. Previous studies have demonstrated how a solar magnetic field placed on the Sun forms a current sheet when magnetic shear is added to the field. Our study is focused on a self-consistent process of how a subsurface magnetic field emerges into the solar atmosphere and forms a current sheet in the corona. This study also gives light to a relation among a flare and two types of flare-associated eruptions; flux-rope eruption and plasmoid eruption.

• 천문학회지
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• 제28권1호
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• pp.77-87
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• 1995

An attempt has been made to analyze time series of $H_\alpha,\;H_\beta,\;and\; H_\gamma$ line profiles taken from a 3B/X6.1 flare which occurred on Oct. 27, 1991 in an active region, NOAA 6891. A total of 22 sets of $H_\alpha,\;H_\beta,\;and\; H_\gamma$ taken with a low and non-uniform time resolution of 10-40 seconds were scanned by PDS with absolute intensity calibration to derive the physical characteristics of the material in the flare chromosphere. Our . results are as follows: (1) The lower Balmer lines observed during the flare activity are broadened by Stark effect. (2) At the peak of the flare activity, the electron temperature of the Balmer line emitting region reaches up to 35000K and its geometrical thickness increases to a scale of $10^4km$, suggesting that high energy particles penetrate deep into the photospheric level.

• 대한가정학회지
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• 제36권2호
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• pp.121-130
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• 1998

The purpose of this study was construction of bell-bottom blue jeans according to change of flare line and investigate the effects clothing pressure according to various movements of the legs. In this study, movements of leg were classified by M1, M2, M3, M4.(M1:erecting, M2: leapfrogging position, M3:sit-on-one' keens position, M4:Traditional nobel-sitting position) The results were as follows: As usings the leg surface shell by the adhesive paper taping method, basic slacks pattern and blue jeans patterns according to change of flare line was constructed. The order of clothing pressure of the different patterns is C(the flare line is on the calf of the leg)>B(the flare line is on the knee)>A(the flare line is on the thigh). Clothing pressure in the knee point was highest and when the flare line was on the calf of the leg, clothing pressure showed high.

• 천문학회지
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• 제33권2호
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• pp.123-126
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• 2000

We have developed a near real-time flare alerting system which (1) downloads the latest GOES-l0 1-8 ${\AA}$ X-ray flux 1-min data by an automated ftp program and shell scripts, (2) produces a beep sound in a simple IDL widget program when the flux is larger than a critical value, and (3) makes it possible to do a wireless alerting by a set of portable transceivers. Thanks to the system, we have made successful Ha flare observations by the Solar Flare Telescope in Bohyunsan Optical Astronomy Observatory. This system is expected to be helpful for ground-based flare observers.

• 천문학회보
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• 제37권2호
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• pp.126.2-126.2
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• 2012

최근 태양 극대기를 맞아 우주기상의 변화에 대처하기 위한 연구가 많이 진행되고 있다. 본 연구에서도 저 중위도 이온권 모델인 SAMI2와 SAMI3를 이용하여 solar flare 발생에 따른 이온권의 변화를 지켜보고자 하였다. 하지만 SAMI 모델에서는 F74113 Solar EUV reference spectrum을 이용하여 EUV flux에 의한 이온화만 고려되었을 뿐, X-ray flux에 의한 이온화는 고려되지 않았다. 태양 극대기동안 solar flare가 발생하였을 때, solar X-ray가 전리층에 미치는 영향이 매우 중요한만큼 solar X-ray에 의한 이온권의 변화를 적용시킬 필요가 있었다. 따라서 우리는 보다 정확한 solar flare 발생에 따른 이온권의 변화를 보기 위해 $1{\AA}{\sim}8{\AA}$범위의 X-ray관측자료를 제공하는 GOES 위성의 데이터를 직접 이용하고, 해당하는 파장의 cross section을 추가하여 SAMI 모델에 적용시켰다. solar flare 효과를 선택적으로 활용하는 개정된 SAMI 모델을 통해 각 flare 등급과 지속시간에 따른 이온권의 변화를 모델로써 확인하였다.

• 천문학회지
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• 제29권spc1호
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• pp.317-319
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• 1996

Utilizing a Calcium filter, a large two ribbon flare of an importance 2.5Xj31? was recorded at. King Abdul-Aziz University Solar Observatory (KAAUSO) at the 30th of October 1991. This chromosphenc flare observation, which is of special importance since it is rarely reported, was for a flare that occurred near the south west of the equator at the vicinity of a large sunspot group on an active region known as AR 6891. The observed foot points of this flare had a strange behavior in which the separating motion of the ribbons were not typical of most flares, rather were nearly orthogonal. In this article we present the characteristics of the main sunspot group of this active region and try to investigate its evolution and fragmentation with time. Information regarding magnetic fields and velocity fields are necessary to understand the restructuring of the magnetic field pattern and plasma motion, and hence the changes that could lead to the occurrence of such an interesting flare.

• Clinical and Experimental Reproductive Medicine
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• 제34권2호
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• pp.125-131
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• 2007

목 적: 난소 반응이 저하된 환자에서 GnRH agonist flare up protocol과 GnRH antagonist protocol의 효용성을 비교하고자 하였다. 연구방법: 2003년 1월부터 2005년 8월까지 체외수정시술을 받은 환자들 가운데 이전의 체외수정시술 주기에서 5개 이하의 난자가 채취되고 기저 FSH 농도가 12 mIU/ml 이상인 총 144명 가운데 73명은 GnRH agonist flare up요법을 사용하였고 71명은 GnRH antagonist 요법을 사용하였다. 양군간에 주기의 취소율, 채취된 난자수, 양질의 수정란의 수, 착상율, 임신율, 출산율을 비교하였다. 결 과: 각 군간에 나이는 평균 37.4세와 38.1세로 antagonist group에서 높았으나 통계학적 유의성은 없었다. 그 외에 기저 FSH 농도와 이전 주기의 취소율도 통계학적 유의성은 없었다. GnRH agonist flare up 주기와 GnRH antagonist 주기에서 취소율은 각각 30.1%, 53.5%로 GnRH antagonist protocol에서 유의 있게 높게 나타났다. 채취된 난자수도 각각 4.18개와 2.16개로 차이를 보였으며 난소 과자극 기간은 각각 10.5일과 9.2일로 antagonist protocol에서 약간 낮은 모습을 보였다. 최고 혈중 E$_2$의 농도와 good embryo 개수도 GnRH agonist flare up요법에서 유의 있게 높게 나타났다. 각 군에서의 착상율, 이식 주기당 임신율, 이식 주기당 출생율은 GnRH agonist flare up요법에서 약간 높은 경향을 보이기는 하였으나 통계학적인 유의성은 없었다. 결 론: 두 군간의 비교에서 GnRH agonist flare up 요법이 시작 주기당 임신율, 출산율에서 높은 경향을 보였으나 통계학적 의의는 없었다. 하지만 난소기능이 저하된 환자에서 난자의 채취 개수는 GnRH agonist flare up 요법이 GnRH antagonist를 사용한 주기보다 의의있게 높게 나타났다. 이러한 연구 결과로 볼 때 저 반응군에 있어서 GnRH antagonist flare up요법이 저 반응군에 있어 향상된 난소 반응을 기대할 가능성이 높을 것으로 생각된다.