• Proceedings of the Korean Society of Disaster Information Conference
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• 2023.11a
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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.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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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.

• The Bulletin of The Korean Astronomical Society
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• v.41 no.2
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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.

• The Bulletin of The Korean Astronomical Society
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• v.40 no.1
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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.

• Journal of The Korean Astronomical Society
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• v.28 no.1
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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.

• Journal of the Korean Home Economics Association
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• v.36 no.2
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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.

• Journal of The Korean Astronomical Society
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• v.33 no.2
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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.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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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.

• Journal of The Korean Astronomical Society
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• v.29 no.spc1
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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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• v.34 no.2
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• pp.125-131
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• 2007

Objective: The aim of this study was to compare GnRH antagonist and agonist flare-up treatment in the management of poor responder patients. Methods: One hundred forty-four patients from Jan. 1, 2002 to Aug. 31, 2005 undergoing IVF/ICSI treatment who responded poorly to the previous cycle (No. of oocyte retrieved$\leq$5) and had high early follicular phase follicle stimulating hormone (FSH>12 mIU/ml were selected. Seventy-five patients received agonist flare-up protocol and 71 patients received antagonist protocol. We analyzed the number of oocytes retrieved, number of good embryos (GI, GI-1), total dose of hMG administered, implantation rate, cycle cancellation rate, pregnancy rate, live birth rate. Results: The cancellation rate was high in antagonist protocol (53.5% vs. 30.1%). The number of oocyte retrieved, the number of good embyos were high in agonist flare-up group. There was no statistical difference between GnRH agonist flare up protocol and GnRH antagonist protocol in implantation rate (14.5%, 10.1%), clinical pregnancy rate per transfer (29.4%, 21.2%) and live birth rate per transfer (21.6%, 18.2%). Although the result was not statistically significant, GnRH agonist flare up group showed a nearly doubled pregnancy rate and live birth rate per initial cycle than GnRH antagonist group. Conclusions: The agonist flare-up protocol appears to be slightly more effective than the GnRH antagonist protocol in implantation rate, pregnancy rate, live birth rate but shows statistically no significance. Agonist flare-up protocol improved the ovarian response in poor responders. However, based of the result of the study, we can expect improved ovarian response in poor responders by GnRH agonist flare up protocol.