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문용재,윤소윤,박영득,장비호,Moon, Yong-Jae,Yoon, So-Yoon,Park, Young-Deuk,Jang, Be-Ho 한국천문학회 1997 天文學論叢 Vol.12 No.1
In this paper we present a newly improved telescope control software and a newly developed data analysis software package for effective use of the Solar Flare Telescope(SOFT) The telescope control software permits us to make not only auto tacking of the SOFT, but also quantitative measurement of the solar irradiation, allowing us to provide weather monitorings. In addition we introduce an IDL widget software package for both monochromatioc (MONO version) and polarimetric data (VMG version) analysis. The MONO version is capable of loading FITS files, changing colors and contrast, image processing, displaying plots, and saving displayed plots by selected formats The VMG version, on the other hand provides a calibration of polarimetric data and plots of reduced vector magnetic fields.
알칼리 환경에 대한 GFRP 복합재료의 내구성에 관한 연구 (1)
문용재(YONG-JAE MOON),박창호(CHANG-HO PARK),문창권(CHANG-KWON MOON) 한국해양공학회 2008 韓國海洋工學會誌 Vol.22 No.1
The effect of alkaline environmental condition on durability of GFRP composites according to additives was investigated. Additives used were polyvinyl alcohol (PVA), kaolin and alumina powder. Weight gains increased with immersion time in all GFRP composites at 80℃ But weight gain of specimen added PVA did not differ through the whole immersion time in both tap water and alkaline solution at 20 and 80℃. Tensile strength decreased with immersion time in all environment conditions. Tensile strength of GFRP composites regardless of additives decreased rapidly up to 5 days of immersion and then decreased slowly up to 30 days in alkaline solution environment at 80 ℃. Weight gains had not much difference in both tap water and alkaline solution at 20 ℃. And weight gain of GFRP composites added polyvinyl alcohol had smaller than the others through the whole immersion time in both tap water and alkaline solution at 20 ℃ and 80 ℃. Tensile strength of GFRP composites added polyvinyl alcohol had higher than the others through the whole immersion time in both tap water and alkaline solution at 20 ℃ and 80 ℃.
Comparison of the WSA-ENLIL CME propagation model with three cone types and an empirical model
장수정,문용재,나현옥,Jang, Soojeong,Moon, Yong-Jae,Na, HyeonOck 한국천문학회 2012 天文學會報 Vol.37 No.2
We have made a comparison of the WSA-ENLIL CME propagation model with three cone types and an empirical model using 29 halo CMEs from 2001 to 2002. These halo CMEs have cone model parameters from Michalek et al. (2007) as well as their associated interplanetary (IP) shocks. For this study we consider three different cone models (an asymmetric cone model, an ice-cream cone model and an elliptical cone model) to determine CME cone parameters (radial velocity, angular width and source location), which are used for input parameters of the WSA-ENLIL CME propagation model. The mean absolute error (MAE) of the arrival times at the Earth for the elliptical cone model is 10 hours, which is about 2 hours smaller than those of the other models. However, this value is still larger than that (8.7 hours) of an empirical model by Kim et al. (2007). We are investigating several possibilities on relatively large errors of the WSA-ENLIL cone model, which may be caused by CME-CME interaction, background solar wind speed, and/or CME density enhancement.
Near-real time Kp forecasting methods based on neural network and support vector machine
지은영,문용재,박종엽,이동훈,Ji, Eun-Young,Moon, Yong-Jae,Park, Jongyeob,Lee, Dong-Hun 한국천문학회 2012 天文學會報 Vol.37 No.2
We have compared near-real time Kp forecast models based on neural network (NN) and support vector machine (SVM) algorithms. We consider four models as follows: (1) a NN model using ACE solar wind data; (2) a SVM model using ACE solar wind data; (3) a NN model using ACE solar wind data and preliminary kp values from US ground-based magnetometers; (4) a SVM model using the same input data as model 3. For the comparison of these models, we estimate correlation coefficients and RMS errors between the observed Kp and the predicted Kp. As a result, we found that the model 3 is better than the other models. The values of correlation coefficients and RMS error of the model 3 are 0.93 and 0.48, respectively. For the forecast evaluation of models for geomagnetic storms ($Kp{\geq}6$), we present contingency tables and estimate statistical parameters such as probability of detection yes (PODy), false alarm ratio (FAR), bias, and critical success index (CSI). From a comparison of these statistical parameters, we found that the SVM models (model 2 and model 4) are better than the NN models (model 1 and model 3). The values of PODy and CSI of the model 4 are the highest among these models (PODy: 0.57 and CSI: 0.48). From these results, we suggest that the NN models are better than the SVM models for predicting Kp and the SVM models are better than the NN models for forecasting geomagnetic storms.
이강진,문용재,이진이,이경선,나현옥,김해연,신대윤,Lee, Kangjin,Moon, Yong-Jae,Lee, Jin-Yi,Lee, Kyoung-Sun,Na, Hyeonock,Kim, Haeyeon,Shin, Dae-Yun 한국천문학회 2012 天文學會報 Vol.37 No.2
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.
박영득,문용재,장비호,심경진,Park, Young-Deuk,Moon, Yong-Jae,Jang, Be-Ho,Sim, Kyung-Jin 한국천문학회 1997 天文學論叢 Vol.12 No.1
SOFT($\underline{So}lar\;\underline{F}lare\;\underline{T}elescope$) installed at BOAO(Bohyunsan Optical Astronomy Observatory) is purposed for observing solar active regions using four refractors on single mount with a $400"\times300"$ field of view: Two refractors with a diameter of 15cm(f15) are observe the white light and $H\alpha$, and the other two refractors with a diameter of 20cm(f8) are observe the magnetic field distribution and Doppler shifts at the solar chromosphere. Three Lyot filters, one of the most important observational instruments, are installed on the optical rails for VMG, LMG, and $H\alpha$ that possible to very narrow pass band observation under high precision stability of temperature. From the combination of KD*P and quarter wave plate in the Lyot filter possible observe the magnetic fields strength and doppler shifts by using the characteristics of polarization components. In this paper, we introduce the basic characteristics, optical system, and monitor system of the SOFT.
CCD 분광 관측에 의한 활동홍염의 도플러 시선속도분포 연구
박영득,윤홍식,문용재,PARK YOUNG DEUK,YUN HONG SIK,MOON YONG-JAE 한국천문학회 1998 天文學論叢 Vol.13 No.1
To study kinematics of solar prominences, we have made Ha spectrographic study of an eruptive prominence which appeared on the 27th of August, 1992 with a position angle of 270 deg. The observation was carried out by a Littrow type spectrograph and a G1 CCD camera attached to the 25cm coronagraph at Norikura Coronal Station. In taking the spectral data the slit was placed in parallel to the solar limb at 7 different heights, each being separated by 5 arcsec with a time step of 30 sec. The observed eruptive prominence shows a wide range of line of sight Doppler velocity, spanning from $V_{dopp}=-17.5km/s\;to\;V_{dopp}=58.2km/s$. It is also found that the velocity increases with height at the rate of ${\Delta}V= 0.86 km/s/arcsec$.
박영득,윤홍식,문용재,PARK YOUNG DEUK,YUN HONG SIK,MOON YONG-JAE 한국천문학회 1998 天文學論叢 Vol.13 No.1
A quantitative analysis has been made to estimate the horizontal variation of physical parameters in a loop type active prominence by analyzing Call H&K and $H_{\varepsilon}{\ldots}$ spectra taken from such an active prominence (appeared on May 23, 1981 with position angle 251 degree) with Littrow type spectrograph attached to 25cm coronagraph at Norikura Coronal Station of National Astronomical Observatory of Japan. The spectral resolution is 1.12A/mm and the spatial resolution is 25'/mm for Call H&K lines. The present study shows that the turbulent velocity ranges from 10km/s to 20 km/s in the loop prominence, which are in good agreement with those of Hirayama (1989). It is also found that the temperature of the loop prominence is higher than that of quiescent prominences$(\~8,000 K)$ by about 4,000 K, whose temperature deviation seems very high.
박영득,윤홍식,문용재,PARK YOUNG DEUK,YUN HONG SIK,MOON YONG-JAE 한국천문학회 1998 天文學論叢 Vol.13 No.1
The size of fine structures in the quiescent prominence that appeared on August 16, 1992 has been estimated using power spectra generated from intensity variations of Ha images of the lower part of the prominence, which were taken with a G1 CCD camera attached to 25cm coronagraph at Norikura Coronal Station in Japan. The lower part of the prominence has shown a distinct intensity variation with optical thickness of $\tau=1\~5$. Our analysis yields a mean size of fine structures ranging from 350 km to 1,000 km, in good agreement with Hirayama(1985) and Zirker & Koutchmy(1989, 1991).