• The Bulletin of The Korean Astronomical Society
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• v.39 no.2
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• pp.97.2-97.2
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• 2014

In this paper, we study the stability and dynamics of a magnetic field producing the M6.6 class solar flare taking place in NOAA active region (AR) 11158 on 2011 February 13th. Toriumi et. al. (2013) recently suggest that a fine scale magnetic structure on the photosphere gives a major possibility to produce the M6.6 class flare. On the other hand, they don't discuss the torus instability as a plausible mechanism even though Zhao et. al. (2014) and Janvier et. al. (2014) suspect it as the trigger mechanism of X2.2 class flare taking place later in the same AR. We are the first to investigate the stability of a nonlinear force-free field (NLFFF) prior to the M6.6 class flare against the torus instability by using analytical and numerical approaches. Consequently, we found that our NLFFF is quite stable against small perturbation. This result supports that the flare is triggered by the photospheric motion suggested by Toriumi et. al. (2013). We further perform another MHD simulation with an anomalous resistivity using the NLFFF as an initial condition. As a result, we found the eruption of strongly twisted lines. We compare our simulation results with observations and discuss relevant dynamics in detail.

• The Journal of Korean Institute of Communications and Information Sciences
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• v.26 no.12A
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• pp.1990-1999
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• 2001

This paper presents a dynamic simulation loop that gives tracking results of 2-color concentric annular ring (CAR) reticle seeker. Our simulation tool includes the target/flare model and a proportional navigation guidance (PNG) loop. The CAR reticle system performances and the flare effects are analyzed in various scenarios. When a flare is present in the field of view (FOV), the simulation results show that the reticle seeker cannot keep a precise target tracking. In this paper, we propose 2-color counter-countermeasure (CCM) using the least mean square (LMS) method to cope with a presence of IR flare. The proposed method makes a simultaneous process in two infrared (IR) wavelength bands: MWIR add SWIR. The simulation results have shown that our adaptive IRCCM algorithm can achieve an effective cancellation of the flare signal with a relatively high intensity.

• Journal of Fashion Business
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• v.1 no.4
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• pp.49-54
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• 1997

Methods of the flare skirt pattern making are presented variously among foreign and domestic test books. Three of them are : First the method is using the basic skirt pattern, secondly the method is quartering rectangle of skirt length $\times\frac{W}4$, finally the method is substituting waist size for formula. But, these books don't include the calculating method of the hem circumference. This calculating method express the shape of flare skirt and the using length of trimming -race and frill-. This study aims at proposing the calculating formula of the hem circumference and the standardization of pattern making technical skill. The result were as follows. 1. The calculating formula of hem circumference had regular ratio in $180^{\circ}$, $270^{\circ}$ and $360^{\circ}C$ flare. That was (HEM) = $(\frac{(5\;{\times}\;(W\;+\;1)}{4\;{\times}\;A}+(SK.L))\;{\times}\;A\;{\times}\;0.785$. A was 4 in $180^{\circ}$, 6 in $270^{\circ}$, 8 in $360^{\circ}$. 2. The error of hem circumference from 46 to 86 centimeter of waist size was between 0.11875 and -0.63125 centimeter in $180^{\circ}$, $270^{\circ}$ and $360^{\circ}$ flare skirt. This formula was less in the error.

• Journal of the Society of Naval Architects of Korea
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• v.44 no.3 s.153
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• pp.279-284
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• 2007

As a container vessel becomes larger, the bow flare becomes larger. The large bow flare structures are often subjected to dynamic pressure loads due to bow flare slamming occurring in rough seas. The aim of this paper is to investigate the characteristics of bow flare slamming pressure measured in a real voyage through the North Pacific Ocean. The characteristics of impact pressure load caused by slamming is addressed in terms of the pressure pulse-time history which involves rising time, peak pressure, decaying time and type of pressure decay. The values were presented using non-dimensional parameters.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.1
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• pp.29.2-29.2
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• 2011

Although stellar flares have a long history of observations, there are few concrete understanding about underlying physical processes and meaningful correlations with other stellar properties. Most of previous observations dealt with only a small number of sample stars, and therefore not sufficient to support generalized statistical studies. Based on one-month long MMT time-series observations of the open cluster M37, we monitored light variations of nearly 2,500 M-dwarf stars and successfully identified 606 flare events from 422 stars. This is a rare attempt to estimate true flare rates and properties among many stars of the same age and mass group. For each flare, we considered both observational and physical parameters including flare shape, duration before and after the peak, baseline magnitude before and after the peak, peak magnitudes, total energy and peak energy, etc. We find significant correlations between some of key parameters over a wide range of energy ($Er=10^{32}{\sim}10^{36}ergs$). For instance, regardless of stellar luminosities, the energy power spectrum of flares can be approximated by a power law (${\beta}=0.83-0.97$). This suggests that flares follow similar physical mechanisms for atmospheric heating and cooling among these low-mass stars. From this MMT data set, we derived an average flaring rate of $0.019 hr^{-1}$ among flare stars and $0.003 hr^{-1}$ for all M-dwarf candidates. We will report the details of our analysis and discuss physical implications.

• Journal of the Society of Naval Architects of Korea
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• v.40 no.3
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• pp.22-28
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• 2003

In rough seas, bow-flare regions of the full ships (tanker and bulk carrier) are subiect to high impact pressures due to the on-coming breaking waves. And many ships suffer structural damages in that region, even though they were built under the bow structure strengthening rules of the ship classes. So, a new design method for bow-flare structure is highly required. In this paper, a new prediction method of the bow-flare impact pressure (in terms of equivalent static pressure) acting on the full ships' bow is presented. This method is based on the 6 full ships' damage analysis and the breaking wave impact mechanism. Calculation results of the bow-flare impact pressure and the shell plate thickness are shown and discussed. Through the example calculations, it was found that the present method is useful for the structure design of the full ships' bow.

• Journal of Korean Society of Transportation
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• v.28 no.6
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• pp.25-32
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• 2010

This study deals with the roundabout by flare of entry and exit. The goal is to analyze the relative effectiveness of roundabout by flare of entry and exit. In pursuing the above, this study gives the particular attentions to comparing the performances using VISSIM software. The main results analyzed are as follows. First, the single and double roundabouts are analyzed to have LOS F in the case of total entering vehicles of 2,400pcph and 4,400pcph Second, the roundabouts by entry flare analyzed to have LOS F in the case of total entering vehicles of 2,800~3,200pcph and the roundabouts by entry and exit flare analyzed to have LOS F in the case of total entering vehicles of 3,200~3,600pcph. Finally, result of comparative analysis of roundabout and roundabout by flare of entry and exit, capacity of roundabout by flare of entry and exit are located between 1-lane roundabout and 2-lane roundabout. therefore it analyzed that roundabout by flare of entry and exit can be added to new type roundabout.

• The Bulletin of The Korean Astronomical Society
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• v.42 no.2
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• pp.59.5-60
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• 2017

We present the relationship between vector magnetic field parameters and solar major flare occurrence rate. Based on this, we are developing a forecast model of major flare (M and X-class) occurrence rate within a day using hourly vector magnetic field data of Space-weather HMI Active Region Patch (SHARP) from May 2010 to April 2017. In order to reduce the projection effect, we use SHARP data whose longitudes are within ${\pm}60$ degrees. We consider six SHARP magnetic parameters (the total unsigned current helicity, the total photospheric magnetic free energy density, the total unsigned vertical current, the absolute value of the net current helicity, the sum of the net current emanating from each polarity, and the total unsigned magnetic flux) with high F-scores as useful predictors of flaring activity from Bobra and Couvidat (2015). We have considered two cases. In case 1, we have divided the data into two sets separated in chronological order. 75% of the data before a given day are used for setting up a flare model and 25% of the data after that day are used for test. In case 2, the data are divided into two sets every year in order to reduce the solar cycle (SC) phase effect. All magnetic parameters are divided into 100 groups to estimate the corresponding flare occurrence rates. The flare identification is determined by using LMSAL flare locations, giving more numbers of flares than the NGDC flare list. Major results are as follows. First, major flare occurrence rates are well correlated with six magnetic parameters. Second, the occurrence rate ranges from 0.001 to 1 for M and X-class flares. Third, the logarithmic values of flaring rates are well approximated by two linear equations with different slopes: steeper one at lower values and lower one at higher values. Fourth, the sum of the net current emanating from each polarity gives the minimum RMS error between observed flare rates and predicted ones. Fifth, the RMS error for case 2, which is taken to reduce SC phase effect, are smaller than those for case 1.

• The Bulletin of The Korean Astronomical Society
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• v.46 no.1
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• pp.42.1-42.1
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• 2021

In this study, we present a visual explanation of a deep learning solar flare forecast model and its relationship to physical parameters of solar active regions (ARs). For this, we use full-disk magnetograms at 00:00 UT from the Solar and Heliospheric Observatory/Michelson Doppler Imager and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager, physical parameters from the Space-weather HMI Active Region Patch (SHARP), and Geostationary Operational Environmental Satellite X-ray flare data. Our deep learning flare forecast model based on the Convolutional Neural Network (CNN) predicts "Yes" or "No" for the daily occurrence of C-, M-, and X-class flares. We interpret the model using two CNN attribution methods (guided backpropagation and Gradient-weighted Class Activation Mapping [Grad-CAM]) that provide quantitative information on explaining the model. We find that our deep learning flare forecasting model is intimately related to AR physical properties that have also been distinguished in previous studies as holding significant predictive ability. Major results of this study are as follows. First, we successfully apply our deep learning models to the forecast of daily solar flare occurrence with TSS = 0.65, without any preprocessing to extract features from data. Second, using the attribution methods, we find that the polarity inversion line is an important feature for the deep learning flare forecasting model. Third, the ARs with high Grad-CAM values produce more flares than those with low Grad-CAM values. Fourth, nine SHARP parameters such as total unsigned vertical current, total unsigned current helicity, total unsigned flux, and total photospheric magnetic free energy density are well correlated with Grad-CAM values.

• The Research Journal of the Costume Culture
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• v.17 no.3
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• pp.472-483
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• 2009

The purpose of this study is to analyse the effects of knit samples' mechanical properties on changes of skirt length of knit flared skirt, and to compare it to the knitting method of a seamless knitted flare skirt. So, I compared the appearance and 3-dimensional shape of a seamless knitted flare skirt with those of a fully cut knit flared skirt. For this study, 18 kinds of cut and sew or seamless knitted test garment were made. The data analysis methods used in this study were descriptive statistics, one-way ANOVA, correlation analysis, and regression analysis. The results are as follows: The result of the evaluation of knit samples' mechanical properties by the KES-FB system showed that elongation decreased as gauge increased and course direction was greatest among grain directions. The length change after wearing the knitted flare skirts appeared wholly equal to the seamless knitted, compared with the cut and sew. The change was biggest at $180^{\circ}$, 7G of the cut and sew. In grain direction, bias cut showed more than 1.2cm of length change. As the weight and thickness increased, the length changes become larger. The regression analysis indicated that the greatest contributive variables on the length changes were elongation, weight, and thickness.