• 천문학회지
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• 제36권spc1호
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• pp.45-47
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• 2003

A white light flare was observed at the limb on 16 August 1989 in He 10830 ${\AA}$ spectra, H$\alpha$ slit jaw photo-grams, and white light filter-grams of ${\lambda}=5600{\AA}{\pm}800{\AA}$. The kernels of the white light flare are not spatially related with Ha brightenings, suggesting that the flare energy would be released at the photosphere.

• 천문학회지
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• 제36권spc1호
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• pp.49-54
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• 2003

We introduce the two-dimensional spectral observations of solar flares using the Solar Tower Tele-scope of Nanjing University, China. In particular, we introduce three typical events and the methods used to analyze the data. (1) The flare of November 11, 1998, which is a limb flare. We derive the temperature and density within the flaring loop using non-LTE calculations. The results show that the loop top may be hotter and denser than other parts of the loop, which may be a result of magnetic reconnect ion above the loop. (2) The flare of March 10, 2001, which is a white-light flare that shows an emission enhancement at the near infrared continuum. We propose a model of non-thermal electron beam heating plus backwarming to interpret the observations. (3) The flare of September 29, 2002, which shows unusual line asymmetries at one flare kernel. The line asymmetries are caused by an upward moving plasma that is accelerated and heated during the flare development.

• 천문학회지
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• 제29권spc1호
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• pp.321-322
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• 1996

Using the data on the occurrences of the Ho: and soft X-ray flares for the time interval of January 1, 1986-May :31, 1994, we have studied the middle term(30-300days) pericities of the solar flare production during the activity cycle 22. Power analysis of the time seies of daily H$\alpha$ flare index in the northern hemisphere shows prominent periodicities at 220, 120, 109, and 92 days(see Figures l(a) and l(b)), while in the southern hemisphere, those at 267, 213, 183, 167, and 107 days are apparent, though their peaks are not so distint as those in the northern hemisphere. Periodogram of daily soft X-ray flare index also reveal the periodicities at 279, 205, 164, 117, and 91 days in the northern hemisphere, and at 266, 220, 199, 162, 120, and 100 days in the southern hemisphere. Howeer, the 155-day periodicity reported for the earlier cycles, 19, 20, and 21, could not be confirmed in our analysis. to be submitted to Solar Physics; an extended abstract.

• 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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• 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.

• 천문학회지
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• 제29권spc1호
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• pp.323-324
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• 1996

In the present work we introduce a new flare activity indicator, MAD and examine its characteristics by analyzing a set of successive three days' observations of a typical active region, AR2372. The computed MAD is compared with conventional activity indicator such as separator. It is found that. (1) MAD traces very well the separator, (2) it. singles out. local discontinuity of magnetic field lines and (3) it. is a good measure of describing the evolutionary status of active region.

• 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.

• 천문학회지
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• 제52권4호
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• pp.133-144
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• 2019

We develop forecast models of daily probabilities of major flares (M- and X-class) based on empirical relationships between photospheric magnetic parameters and daily flaring rates from May 2010 to April 2018. In this study, we consider ten magnetic parameters characterizing size, distribution, and non-potentiality of vector magnetic fields from Solar Dynamics Observatory (SDO)/Helioseismic and Magnetic Imager (HMI) and Geostationary Operational Environmental Satellites (GOES) X-ray flare data. The magnetic parameters are classified into three types: the total unsigned parameters, the total signed parameters, and the mean parameters. We divide the data into two sets chronologically: 70% for training and 30% for testing. The empirical relationships between the parameters and flaring rates are used to predict flare occurrence probabilities for a given magnetic parameter value. Major results of this study are as follows. First, major flare occurrence rates are well correlated with ten parameters having correlation coefficients above 0.85. Second, logarithmic values of flaring rates are well approximated by linear equations. Third, using total unsigned and signed parameters achieved better performance for predicting flares than the mean parameters in terms of verification measures of probabilistic and converted binary forecasts. We conclude that the total quantity of non-potentiality of magnetic fields is crucial for flare forecasting among the magnetic parameters considered in this study. When this model is applied for operational use, it can be used using the data of 21:00 TAI with a slight underestimation of 2-6.3%.

• 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.

• 천문학회지
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• 제36권2호
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• pp.61-66
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• 2003

We have examined the relationship between the speeds of coronal mass ejections (CMEs) and the GOES X-ray peak fluxes of associated flares. Noting that previous studies were possibly affected by projection effects and random association effects, we have considered two sets of carefully selected CME-flare events: four homologous events and four well-observed limb events. In the respective samples, good correlations are found between the CME speeds and the GOES X-ray peak fluxes of the associated flares. A similarly good correlation is found for all eight events of both samples when the CME speeds of the homologous events are corrected for projection effect. Our results suggest that a close relationship possibly exists between CME kinematics and flaring processes.